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C 477.3 



XVIII. Catalogue of 500 new Nebula, nebulous Stars, planetary 
Nebula, and Clusters of Stars ; with Remarks on the Con- 
struction of the Heavens. By William Herschel, LL. D. 
F. R. S. 

Read July 1, 1802. 

oince the publication of my former two catalogues of nebulse, 
I have, in the continuation of my telescopic sweeps, met with a 
number of objects that will enrich our natural history, as it 
may be called, of the heavens. A catalogue of them will be 
found at the end of this paper, containing 500 new nebulae, 
nebulous stars, planetary nebulse, and clusters of stars. These 
objects have been arranged in eight classes, in conformity 
with the former catalogues, of which the present one is there- 
fore a regular continuation. This renders it unnecessary to give 
any further explanation, either of the contents of its columns, or 
the abbreviations which have been used in the description of 
the objects. 

It has hitherto been the chief employment of the physical 
astronomer, to search for new celestial objects, whatsoever might 
be their nature or condition ; but our stock of materials is now 
so increased, that we should begin to arrange them more scien- 
tifically. The classification adopted in my catalogues, is little 
more than an arrangement of the objects for the convenience 
of the observer, and may be compared to the disposition of the 
books in a library, where the different sizes of the volumes is 

mdcccii. 3 Q 



478 Tk. Herschel's Catalogue 

often more considered than their contents. But here, in dividing 
the different parts of which the sidereal heavens are composed 
into proper classes, I shall have to examine the nature of the 
various celestial objects that have been hitherto discovered, in 
order to arrange them in a manner most conformable to their 
construction. This will bring on some extensive considerations, 
which would be too long for the compass of a single paper; I 
shall therefore now only give an enumeration of the species 
that offer themselves already to our view, and leave a particular 
examination of the separate divisions, for some early future 
occasions. 

In proceeding from the most simple to the more complex 
arrangements, several methods, taken from the known laws of 
gravitation, will be suggested, by which the various systems 
under consideration may be maintained ; but here also we shall 
confine ourselves to a general review of the subject, as obser- 
vation must furnish us first with the necessary data, to establish 
the application of any one of these methods on a proper 
foundation. 

ENUMERATION OF THE PARTS THAT ENTER INTO THE CONSTRUC- 
TION OF THE HEAVENS. 

I. Of insulated Stars. 

In beginning our proposed enumeration, it might be expected 
that the solar system would stand foremost in the list ; whereas, 
by treating of insulated stars, we seem, as it were, to overlook one 
of the great component parts of the universe. It will, however, 
soon appear that this very system, magnificent as it is, can only 
rank as a single individual belonging to the species which we 
are going to consider. 



of 500 nevo Nebula, and Clusters of Stars. 479 

By calling a star insulated, I do not mean to denote its being 
totally unconnected with all other stars or systems ; for no one, 
by the laws of gravitation, can be intirely free from the in- 
fluence of other celestial bodies. But, when stars are situated at 
such immense distances from each other as our sun, Arcturus, 
Capella, Lyra, Sirius, Ganobus, Markab, Bellatrix, Menkar, 
Shedir, Algorah, Propus, and numberless others probably are, 
we may then look upon them as sufficiently out of the reach of 
mutual attractions, to deserve the name of insulated stars. 

In order not to take this assertion for granted, without some 
examination, let us admit, as is highly probable, that the whole 
orbit of the earth's annual motion does not subtend more than 
an angle of one second of a degree, when seen from Sirius. In 
consequence of this, it appears by computation, that our sun and 
Sirius, if we suppose their masses to be equal, would not fall 
together in less than 33 millions of years, even though they 
were not impeded by many contrary attractions of other neigh- 
bouring insulated stars; and that, consequently, with the 
assistance of the opposite energies exerted by such surrounding 
stars, these two bodies may remain for millions of ages, in a 
state almost equal to undisturbed rest. A star thus situated may 
certainly deserve to be called insulated, since it does not imme- 
diately enter into connection with any neighbouring star; and 
it is therefore highly probable, that our sun is one of a great 
number that are in similar circumstances. To this may be 
added, that the stars we consider as insulated are also sur- 
rounded by a magnificent collection of innumerable stars, called 
the milky-way, which must occasion a very powerful balance 
of opposite attractions, to hold the intermediate stars in a state 
of rest. For, though our sun, and all the stars we see, may 

3Q a 



480 Dr. Herschel's Catalogue 

truly be said to be in the plane of the milky- way, yet I am now 
convinced, by a long inspection and continued examination of 
it, that the milky-way itself consists of stars very differently 
scattered from those which are immediately about us. But of 
this, more will be said on another occasion. 

From the detached situation of insulated stars, it appears that 
they are capable of being the centres of extensive planetary 
systems. Of this we have a convincing proof in our sun, which, 
according to our classification, is one of these stars. Now, as 
we enjoy the advantage of being able to view the solar system 
in all its parts, by means of our telescopes, and are therefore 
sufficiently acquainted with it, there will be no occasion to enter 
into a detail of its construction. 

The question will now arise, whether every insulated star be 
a sun like ours, attended with planets, satellites, and numerous 
comets ? And here, as nothing appears against the supposition, 
we may from analogy admit the probability of it. But, were we 
to extend this argument to other sidereal constructions, or, still 
farther, to every star of the heavens, as has been done fre- 
quently, I should not only hesitate, but even think that, from 
what will be said of stars which enter into complicated sidereal 
systems, the contrary is far more likely to be the case ; and that, 
probably, we can only look for solar systems among insulated 
stars. 

II. Of Binary sidereal Systems, or double Stars. 

The next part in the construction of the heavens, that offers 
itself to our consideration, is the union of two stars, that are 
formed together into one system, by the laws of attraction. 

If a certain star should be situated at any, perhaps immense, 



of 500 new Nebula, and Clusters of Stars. 481 

distance behind another, and but very little deviating from the 
line in which we see the first, we should then have the ap- 
pearance of a double star. But these stars, being totally uncon- 
nected, would not form a binary system. If, on the contrary, 
two stars should really be situated very near each other, and at 
the same time so far insulated as not to be materially affected 
by the attractions of neighbouring stars, they will then compose 
a separate system, and remain united by the bond of their own 
mutual gravitation towards each other. This should be called a 
real double star; and any two stars that are thus mutually 
connected, form the binary sidereal system which we are now 
to consider. 

It is easy to prove, from the doctrine of gravitation, that two 
stars may be so connected together as to perform circles, or 
similar ellipses, round their common centre of gravity. In this 
case, they will always move in directions opposite and parallel 
to each other ; and their system, if not destroyed by some foreign 
cause, will remain permanent. 

Figure 1 (Plate XVI.) represents two equal stars a and b, 
moving in one common circular orbit round the centre 0, but 
in the opposite directions of at and bt. In Fig. 2 we have a 
similar connection of the two stars a b; but, as they are of dif- 
ferent magnitudes, or contain unequal quantities of matter, they 
will move in circular orbits of different dimensions round their 
common centre of gravity 0. Fig. 3 represents equal, and Fig. 4, 
unequal stars, moving in similar elliptical orbits round a com- 
mon centre ; and, in all these cases, the directions of the tangents 
1 1, in the places a b, where the stars are, will be opposite and 
parallel, as will be more fully explained hereafter. 

These four orbits, simple as they are, open an extensive field 



48s Dr. Herschel's Catalogue 

for reflection, and, I may add, for calculation. They shew, even 
before we come to more complicated combinations, where the 
same will be confirmed, that there is an essential difference 
between the construction of solar and sidereal systems. In 
each solar system, we have a very ponderous attractive centre, 
by which all the planets, satellites, and comets are governed, 
and kept in their orbits. Sidereal systems take a greater scope : 
the stars of which they are composed move round an empty 
centre, to which they are nevertheless as firmly bound as the 
planets to their massy one. It is however not necessary here to 
enlarge on distinctions which will hereafter be strongly sup- 
ported by facts, when clusters of stars come to be considered. 
I shall only add, that in the subordinate bodies of the solar 
system itself, we have already instances, in miniature, as it may 
be called, of the principle whereby the laws of attraction are 
applicable to the solution of the most complicated phenomena 
of the heavens, by means of revolutions round empty centres. 
For, although both the earth and its moon are retained in their 
orbits by the sun, yet their mutual subordinate system is such, 
that they perform secondary monthly revolutions round a centre 
without a body placed in it. The same indeed, though under 
very narrow limits, may be said of the sun and each planet 
itself. 

That no insulated stars, of nearly an equal size and distance, 
can appear double to us, may be proved thus. Let Arcturus and 
Lyra be the stars : these, by the rule of insulation, which we 
must now suppose can only take place when their distance from 
each other is not less than that of Sirius from us, if very accu- 
rately placed, would be seen under an angle of 60 degrees from 
each other. They really are at about 59 . Now, in order to 



of 500 new Nebula,, and Clusters of Stars. 483 

make these stars appear to us near enough to come under the 
denomination of a double star of the first class, we should re- 
move the earth from them at least 41353 times farther than 
Sirius is from us. But the space-penetrating power of a 7-feet 
reflector, by which my observations on double stars have been 
made, cannot intitle us to see stars at such an immense distance ; 
for, even the 40-feet telescope, as has been shewn,* can only 
reach stars of the 1343d magnitude. It follows, therefore, that 
these stars could not remain visible in a 7-feet reflector, if they 
were so far removed as to make their angular distance less than 
about 24^ minutes ; nor could even the 40-feet telescope, under the 
same circumstances of removal, shew them, unless they were to 
be seen at least sf- minutes asunder. Moreover, this calculation 
is made on a supposition that the stars of which a double star is 
composed, might be as small as any that can possibly be per- 
ceived ; but if, on the contrary, they should still appear of a 
considerable size, it will then be so much the more evident that 
such stars cannot have any great real distance, and that, con- 
sequently, insulated stars cannot appear double, if they are situ- 
ated at equal distances from us. If, however, their arrangement 
should be such as has been mentioned before, then, one of them 
being far behind the other, an apparent double star may cer- 
tainly be produced ; but here the appearance of proximity 
would be deceptive ; and the object so circumstanced could not 
be classed in the list of binary systems. However, as we must 
grant, that in particular situations stars apparently double may 
be composed of such as are insulated, it cannot be improper to 
consult calculation', in order to see whether it be likely that the 
700 double stars I have given in two catalogues, as well as 

* See Phil. Trans, for 1800, Part I. page 83. 



484 T>r. Herschel's Catalogue 

many more I have since collected, should be of that kind. Such 
an inquiry, though not very material to our present purpose, 
will hereafter be of use to us, when we come to consider more 
complicated systems. For, if it can be shown that the odds are 
very much against the casual production of double stars, the 
same argument will be still more forcible, when applied to treble, 
quadruple, or multiple compositions. 

Let us take £" Aquarii, for an instance of computation. This 
star is admitted, by Flamsteed, De la Caille, Bradley, and 
Mayer, to be of the 4th magnitude. The two stars that com- 
pose it being equal in brightness, each of them may be supposed 
to shine with half the light of the whole lustre. This, according 
to our way of reckoning magnitudes,* would make them 4m 
x y/a = 5fm ; that is, of between the 6th and 5th magnitude 
each. Now, the light we receive from a star being as the square 
of its diameter directly, and as the square of its distance in- 
versely, if one of the stars of £ Aquarii be farther off than the 
stars of between the 6th and 5th magnitude are from us, it must 
be so much larger in diameter, in order to give us an equal 
quantity of light. Let it be at the distance of the stars of the 
7th magnitude; then its diameter will be to the diameter of 
the star which is nearest to us as 7 to 5^, and its bulk as 1,885 
to 1 ; which is almost double that of the nearest star. Then, 
putting the number of stars we call of between the 6th and 
5th magnitude at 450, we shall have 686 of the 7th magnitude 
to combine with them, so that they may make up a double star 
of the first class, that is to say, that the two stars may not be 
more than 5" asunder. The surface of the globe contains 

• The expressions 2m, 3m, 4m, &c. stand for stars at the distance of 2, 3, 4, &c. 
times that of Sirius, supposed unity. 



of 500 new Nebula, and Clusters of Stars. 485 

34036131547 circular spaces, each of 5" in diameter; so that 
each of the 686 stars will have 49615357 of these circles in 
which it might be placed ; but, of all that number, a single one 
would only be the proper situation in which it could make up a 
double star with one of the 450 given stars. But these odds, 
which are above 75! millions to one against the composition of 
g Aquarii, are extremely increased by our foregoing calculation 
of the required size of the star, which must contain nearly 
double the mass allotted to other stars of the 7th magnitude; 
of which, therefore, none but this one can be proper for making 
up the required double star. If the stars of the 8th and 9th 
magnitudes, of which there will be 896 and 1134, should be 
taken in, by way of increasing the chance in favour of the sup- 
posed composition of our double star, the advantage intended to 
be obtained by the addition of numbers, will be completely 
counteracted by the requisite uncommon bulk of the star which 
is to serve the purpose; for, one of the 8th magnitude, ought 
to be more than sf times bigger than the rest; and, if the 
composition were made by a star of the 9th magnitude, no less 
than four times the bulk of the other star which is to enter the 
composition of the double star would answer the purpose of its 
required brightness. Hence therefore it is evident, that casual 
situations will not account for the multiplied phenomena of 
double stars, and that consequently their existence must be 
owing to the influence of some general law of nature ; now, as 
the mutual gravitation of bodies towards each other is quite suf- 
ficient to account for the union of two stars, we are authorised 
to ascribe such combinations to that principle, 

It will not be necessary to insist any further on arguments 
drawn from calculation, as I shall soon communicate a series of 

mdcccii. 3 R 



4§S Br. Herschei/s Catalogue 

observations made on double stars, whereby it will be seen, that 
many of them have actually changed their situation with regard to 
each other, in a progressive course, denoting a periodical revo- 
lution round each other; and that the motion of some of them is 
direct, while that of others is retrograde. Should these observa-* 
tions be found sufficiently conclusive, we may already have their 
periodical times near enough to calculate, within a certain de- 
gree of approximation, the parallax and mutual distance of the 
stars which compose these systems, by measuring their orbits, 
which subtend a visible angle. 

Before we leave the subject of binary systems, I should 
remark, that it evidently appears, that our sun does not enter 
into a combination with any other star, so as to form one of 
these systems with it. This could not take place without our 
immediately perceiving it; and, though we may have good 
reason to believe that our system is not perfectly at rest, yet the 
causes of its proper motion are more probably to be ascribed to 
some perturbations arising from the proper motion of neigh- 
bouring stars or systems, than to be placed to the account of a 
periodical revolution round some imaginary distant centre. 

III. Of more complicated sidereal Systems, or treble, quadruple, 
quintuple, and multiple Stars. 

Those who have admitted our arguments for the existence of 
real double stars, will easily advance a step farther, and allow 
that three stars may be connected in one mutual system of re- 
ciprocal attraction. And, as we have from theory pointed out, 
in figures 1, 2, 3, and 4, how two stars may be maintained 
in a binary system, we shall here shew that three stars may 



of soo new Nebula, and Clusters of Stars. 487 

likewise be preserved in a permanent connection, by revolving 
in proper orbits about a common centre of motion. 

In all cases where stars are supposed to move round an empty 
centre, in equal periodical times, it may be proved that an ima- 
ginary attractive force may be supposed to be lodged in that 
centre, which increases in a direct ratio of the distances. For 
since, in different circles, by the law of centripetal forces, the 
squares of the periodical times are as the radii divided by the 
central attractive forces, it follows, that When these periodical 
times are equal, the forces will be as the radii. Hence we con- 
clude, that in any system of bodies, where the attractive forces 
Of all the rest upon any one of them, when reduced to a direc- 
tion as coming from the empty centre, can be shewn to be in a 
direct ratio of the distance of that body from the centre, the 
system may revolve together without perturbation, and remain 
permanently connected without a central body. 

Hence may be proved, as has been mentioned before, that 
two stars will move round a hypothetical centre of attraction. 
For, let it be supposed that the empty centre 0, in Fig. 1 and 3, 
is possessed of an attractive force, increasing in the direct ratio 
of the distances oa : ob. Then, since here ao and bo are equal, 
the hypothetical attractions will be equal, and the bodies will 
revolve in equal times. That this agrees with the general law 
of attraction, is proved thus. The real attraction of b upon a is 

-"!»-; and that of a upon' b is '-— -; and, since 6 = a, it will be 

-~ : ■—- : : ao\bo ; which was required. 

In Figures 2 and 4, when the stars a and b are unequal, and 
their distances from also unequal, let oa = n, and ob — m; 
and let the mass of matter in a=zm, and in b = ». Then the 

3 R a 



488 Dr. Herschel's Catalogue 

attraction of b on a = —rr, will be to the attraction of a on b 

= — gr, as » : w ; which is again directly as ao : bo. 

I proceed now to explain a combination of three bodies, 
moving round a centre of hypothetical attraction. Fig. 5 con- 
tains a single orbit, wherein three equal bodies a b c, placed at 
equal distances, may revolve permanently. For, the real attrac- 
tion of b on a will be expressed by -~ ; but this, reduced to the 

direction ao, will be only ~~ ; for, the attraction in the direc- 
tion ba is to that in the direction by, parallel to ao, as -^ to 

—~ -. The attraction also of c on a is equal to that of b on a ; 
therefore the whole attraction on a, in a direction towards 0, will 
be expressed by 2b ^ . In the same manner we prove, that the 

attraction of a and c on b, in the direction bo, is ~^r- ; and that 

of a and b on c, in the direction co, is ~cf • Hence, <2 6 and 
£ being equal, the attractions in the directions ao bo and co will 
also be equal ; and, consequently, in the direct ratio of these 
distances. Or rather, the hypothetical attractions being equal, it 
proves that, in order to revolve permanently, a b and c must be 
equal to each other. 

Instead of moving in one circular orbit, the three stars may 
revolve in three equal ellipses, round their common centre of 
gravity, as in Fig. 6. And here we should remark, that this 
centre of gravity will be situated in the common focus 0, of the 
three ellipses ; and that the absolute attraction towards that 
focus, will vary in the inverse ratio of the squares of the distances 
of any one of the stars from that centre, while the relative 
attractions remain in the direct ratio of their several distances 



of 500 new Nebula, and Clusters of Stars. 489 

from the same centre. This will be more fully explained, when 
we come to consider the motion of four stars. 

A very singular straight-lined orbit, if so it may be called, 
may also exist in the following manner. If 4 and b, Fig. 7, are 
two large equal stars, which are connected together by their 
mutual gravitation towards each other, and have such projectile 
motions as would cause them to move in a circular orbit about 
their common centre of gravity, then may a third small star c, 
situated in a line drawn through 0, and at rectangles to the plane 
described by the stars a b, fall freely from rest, with a gradually 
acquired motion to ; then, passing through the plane of the 
orbit of the two stars, it will proceed, but with a gradually re- 
tarded motion, to a second point of rest d; and, in this manner, 
the star c may continue to oscillate between c and d, in a straight 
line, passing from ( , through the centre 0, to d, and back again 
to c. 

In order to see the possibility and permanency of this con- 
nection the better, let be the centre of gravity of the three 
bodies, when the oscillating body is at c ; then, supposing the 
bodies a and b to be at that moment in the plane p I, and ad- 
mitting m to represent a body equal in mass to the two bodies 
a b, will be the common centre of gravity of m and c. Then, 
by the force of attraction, the body c and the fictitious body m 
will meet in ; that is to say, the plane p I, of the bodies a b, 
will now be at p' V. The fictitious body m may then be con- 
ceived to move on till it comes to n, while the body c goes to 
d ; or, which is the same, the plane of the bodies a b will now 
be in the position p" I", as much beyond the centre of gravity 0, 
as it was on the opposite side m. By this time, both the ficti- 
tious body m, now at n, and the real body c, now at d, have lost 



4po Dr. Herschel's Catalogue 

their motion in opposite directions, and begin to approach to 
their common centre of gravity o, in which they will meet a 
second time. It is evident that the orbit of the two large stars 
will suffer considerable perturbations, not only in its plane, but 
also in its curvature, which will not remain strictly circular; 
the construction of the system, however, is such as to contain a 
sufficient compensation for every disturbing force, and will con- 
sequently be in its nature permanent. 

In order to add an oscillating star, it is not necessary that the 
two large stars should be so situated as to move in a circular 
orbit, without the oscillating star. In Fig. 8, the stars a and b 
may have such projectile forces given them as would cause them 
to describe equal ellipses, of any degree of excentricity. If now 
the small star c be added, the perturbations will undoubtedly 
affect not only the plane of the orbits of the stars, but also their 
figures, which will become irregular moveable ovals. The extent 
also of the oscillations of the star f will be affected ; and will 
sometimes exceed the limits c d, and sometimes fall short of 
them. All these varieties may easily be deduced from what has 
been already said, when Fig, 7 was considered. It is however 
very evident, that this system also must be permanent ; since 
not only the centre of gravity will always be at rest, but a 0, 
whatever may be the perturbations arising from the situation of 
c, will still remain equal to b 0. 

It should be remarked, that the vibratory motion of the star c 
will differ much from a cometary orbit, even though the latter 
should be compressed into an evanescent ellipsis. For, while the 
former extends itself over the diameter of a globe in which it 
may be supposed to be inscribed, the hypothetical attractive 
force being supposed to be placed in its centre, the cometary 



of 500 new Nebulce, and Clusters of Stars. 491 

orbit will only describe a radius of the same globe, on account 
of its requiring a solid attractive centre. 

After what has been said, it will hardly be necessary to add, 
that with the assistance of any proper one of the combinations 
pointed out in the four last figures, the appearance of every 
treble star may be completely explained; especially when the 
different inclinations of the orbits of the stars, to the line of sight, 
are taken into consideration. 

If we admit of treble stars, we can have no reason to oppose 
more complicated connections ; and, in order to form an idea 
how the laws of gravitation may easily support such systems, I 
have joined some additional delineations. A very short expla- 
nation of them will be sufficient. 

Fig. 9 ( Plate XVII.) represents four stars, a b c and d, arranged 
in a line; a being equal to b, and c equal to d. Then, if ao = 
bo, and co = do, the centre of gravity will be in ; and, with a 
proper adjustment of projectile forces, the four stars will revolve in 
two circular orbits round their common centre. By calculating 
in the manner already pointed out, it will be found, that when, 
for instance, ao = 1, co = 3, and c = d = 1, then the mass of 
matter in a = b, will be required to be equal to 1,34,92. 

It is not necessary that the projectile force of the four stars 
should be such as will occasion them to revolve in circles. The 
system will be equally permanent when they describe similar 
ellipses about the common centre of gravity, which will also be 
the common focus of the four ellipses. In Fig. 10, the stars 
abed, revolving in ellipses that are similar, will always 
describe, at the same time, equal angles in each ellipsis about the 
centre of hypothetical attraction ; and, when they are removed 
from a b c d to a'b'c'd', they will still be situated in a straight 



493 Dr. Herschei/s Catalogue 

line, and at the same proportionate distances from each other as 
before. By this it appears, as we have already observed, that 
the absolute hypothetical force in the situation a' b' c' d', com- 
pared to what it was when the stars were at abed, is inversely 
as the squares of the distances ; but that its comparative exertion 
on the stars, in their present situation, is still in a direct ratio of 
their distances from the centre o, just as it was when they were 
at a b c d; or, to express the same perhaps more clearly, the 
force exerted on a', is to that which was exerted on a as 
■=£=rr- : =^r . But the force exerted on a is to that exerted 



on c, in our present instance, as ao = 1 to co — g; and still 
remains in the same ratio when the stars are at a' and c' ; for 
the exertion will here be likewise as a'o = 1 to c'o = 3. 

Fig. 11 represents four stars in one circular orbit; and its 
calculation is so simple, that, after what has been said of Fig. 5, 
I need only remark that the stars may be of any size, provided 
their masses of matter are equal to each other. 

It is also evident, that the projectile motion of four equal stars 
is not confined to that particular adjustment which will make 
them revolve in a circle. It will be sufficient, in order to pro- 
duce a permanent system, if the stars abed, in Fig. 12, are 
impressed with such projectile forces as will make them describe 
equal ellipses round the common centre 0. And, as the same 
method of calculation which has been explained with Figs. 6 
and 10 may here be used, it will not be necessary to enter into 
particulars. 

Fig. 13 represents four stars, placed so that, with properly 
adjusted projectile forces, they may revolve in e^ual times, and 
in two different circles, round their common centre of gravity 0, 



of 500 new Nebula, and Clusters of Stars. 493 

If ao = bo = 4, co = do=z 5, and c = c? = 1, then will the 
mass of matter in a — b, required for the purpose, be 1,5136. 
This arrangement, remarkable as it may appear, cannot be 
made in all situations ; for instance, if the distance ao —bo were 
assumed equal to 1, that of co — do being 2, it would be im- 
possible to find such quantities of matter in a and b as would 
unite the four stars into one system. 

As we have shewn how the arrangement in Fig. 10 may be 
derived from that of Fig. 9, so it will equally appear, that four 
stars may revolve in different but similar ellipses round their 
common centre, as in Fig. 14. For here the four stars, when 
placed at abed, are exactly in the situation represented in 
Fig. 13; but, on account of different projectile forces, they re- 
volve, not as before in concentric circles, but in similar elliptical 
orbits. 

Fig. 15 represents three stars, a b c, in the situation of Fig. 5, 
to which a small oscillating star, d, is added. The addition of 
such a star to Fig. 1, has been sufficiently explained in Fig. 7; 
and, what has been remarked there, may easily be applied to 
our present figure. As the fictitious body m, in Fig. 7, was made 
to represent the stars a and b, it will now stand for the three 
stars a b and c. If we suppose these stars to be of an equal 
magnitude in both figures, the centre of gravity 0, of the three 
stars, will not be so far from m and n as in Fig. 7; and the 
perturbations will be proportionally lessened. 

Fig. 16 gives the situation of three stars, a b c, moving in 
equal elliptical orbits about their common focus 0, while the 
star d performs oscillations between d and e. What has been 
said in explaining Fig. 8, will be sufficient to shew, that the 

mdcccii. 3 S 



494 D r ' Herschel's Catalogue 

present arrangement is equally to be admitted among the con- 
structions of sidereal systems that may be permanent. 

We have before remarked, that any appearance of treble 
stars might be explained, by admitting the combinations pointed 
out in Figs. 5, 6, 7, and 8 ; and it must be equally obvious, that 
quadruple systems, under what shape soever they may show 
themselves, whether in straight lines, squares, trapezia, or any 
other seemingly the most irregular configurations, will readily 
find a solution from one or other of the arrangements of the 
eight last figures. 

More numerous combinations of stars may still take place, 
by admitting simple and regular perturbations; for then all 
sorts of erratic orbits of multiple flexures may have a permanent 
existence. But, as it would lead me too far, to apply calculation 
to them, I forbear entering upon the subject at present. 

Before I proceed, it will be proper to remark, that it may 
possibly occur to many, who are not much acquainted with the 
arrangement of the numberless stars of the heavens, that what 
has been said may all be mere useless surmise ; and that, possibly, 
there may not be the least occasion for any such speculations 
upon the subject. To this, however, it may be answered, that 
such combinations as I have mentioned, are not the inventions 
of fancy : they have an actual existence ; and, were it necessary, 
I could point them out by thousands. There is not a single 
night when, in passing over the zones of the heavens by sweep- 
ing, I do not meet with numerous collections of double, treble, 
quadruple, quintuple, and multiple stars, apparently insulated 
from other groups, and probably joined in some small sidereal 
system of their own. I do not imagine that I have pointed out 



of 500 new Nebula, and Clusters of Stars. 495 

the actual manner in which they are held together; but it will 
always be a desirable step towards information, if the possibility 
of such unions, in many different ways, can be laid before us ; 
and, very probably, those who have more leisure to consider the 
different combinations of central forces, than a practical astro- 
nomer can have, may easily enlarge on what has been laid down 
in the foregoing paragraphs. 

IV. Of clustering Stars, and the Milky-way. 

From quadruple, quintuple, and multiple stars, we are na- 
turally led to a consideration of the vast collections of small 
stars that are profusely scattered over the milky-way. On a 
very slight examination, it will appear that this immense starry 
aggregation is by no means uniform. The stars of which it is 
composed are very unequally scattered, and show evident marks 
of clustering together into many separate allotments. By referring 
to some one of these clustering collections in the heavens, what 
will be said of them will be much better understood, than if we 
were to treat of them merely in a general way. Let us take the 
space between j3 and y Cygni for an example, in which the 
stars are clustering with a kind of division between them, so 
that we may suppose them to be clustering towards two different 
regions. By a computation, founded on observations which 
ascertain the number of stars in different fields of view, it ap- 
pears that our space between /3 and y, taking an average breadth 
of about five degrees of it, contains more than 331 thousand 
stars ; and, admitting them to be clustering two different ways, 
we have 165 thousand for each clustering collection. Now, as 
a more particular account of the milky-way will be the subject 
of a separate paper, I shall only observe, that the above mentioned 

3 S a 



49$ Dr. Herschei/s Catalogue 

milky appearances deserve the name of clustering collections, 
as they are certainly brighter about the middle, and fainter 
near their undefined borders. For, in my sweeps of the heavens, 
it has been fully ascertained, that the brightness of the milky- 
way arises only from stars; and that their compression in- 
creases in proportion to the brightness of the milky- way. 

We may indeed partly ascribe the increase, both of brightness 
and of apparent compression, to a greater depth of the space 
which contains these stars ; but this will equally tend to shew 
their clustering condition : for, since the increase of brightness 
is gradual, the space containing the clustering stars must tend 
to a spherical form, if the gradual increase of brightness is to 
be explained by the situation of the stars. 

V. Of Groups of Stars. 

From clustering stars there is but a short transition to groups 
of stars ; they are, however, sufficiently distinct to deserve a 
separate notice. A group is a collection of closely, and almost 
equally compressed stars, of any figure or outline ; it contains 
no particular condensation that might point out the seat of an 
hypothetical central force; and is sufficiently separated from 
neighbouring stars to shew that it makes a peculiar system of its 
own. It must be remembered, that its being a separate system 
does not exclude it from the action or influence of other systems. 
We are to understand this with the same reserve that has been 
pointed out, when we explained what we called insulated stars. 

The construction of groups of stars is perhaps, of all the ob- 
jects in the heavens, the most difficult to explain ; much less 
can we now enter into a detail of the numerous observations I 



of 500 new Nebula, and Clusters of Stars. 497 

have already made upon this subject. I therefore proceed in my 
enumeration. 

VI. Of Clusters of Stars. 

These are certainly the most magnificent objects that can 
be seen in the heavens. They are totally different from mere 
groups of stars, in their beautiful and artificial arrangement : 
their form is generally round ; and the compression of the stars 
shews a gradual, and pretty sudden accumulation towards the 
centre, where, aided by the depth of the cluster, which we can 
have no doubt is of a globular form, the condensation is such, 
that the stars are sufficiently compressed to produce a mottled 
lustre, nearly amounting to the semblance of a nucleus. A 
centre of attraction is so strongly indicated, by all the circum- 
stances of the appearance of the cluster, that we cannot doubt a 
single moment of its existence, either in a state of real solidity, 
or in that of an empty centre, possessed of an hypothetical force, 
arising from the joint exertion of the numerous stars that enter 
into the composition of the cluster. 

The number of 'observations I have to give relating to this 
article, in which my telescopes, especially those of high space- 
penetrating power, have been of the greatest service, of course 
can find no room in this enumeration. 

VII. OfNebulce. 

These curious objects, which, on account of their great dis- 
tance, can only be seen by instruments of great space-pene- 
trating power, are perhaps all to be resolved into the three 
last mentioned species. Clustering collections of stars, for 
instance, may easily be supposed sufficiently removed to present 



4$8 Dr. Herschel's Catalogue 

us with the appearance of a nebula of any shape, which, like 
the real object of which it is the miniature, will seem to be gra- 
dually brighter in the middle. Groups of stars also may, by 
distance, assume the semblance of nebulous patches ; and real 
clusters of stars, for the same reason, when their composition 
is beyond the reach of our most powerful instruments to resolve 
them, will appear like round nebulae that are gradually much 
brighter in the middle. On this occasion I must remark, that 
with instruments of high space-penetrating powers, such as my 
40-feet telescope, nebulas are the objects that may be perceived 
at the greatest distance. Clustering collections of stars, much 
less than those we have mentioned before, may easily contain 
50000 of them ; and, as that number has been chosen for an 
instance of calculating the distance at which one of the most 
remote objects might be still visible,* I shall take notice of an 
evident consequence attending the result of the computation ; 
which is, that a telescope with a power of penetrating into space, 
like my 40-feet one, has also, as it may be called, a power of 
penetrating into time past. To explain this, we must consider 
that, from the known velocity of light, it may be proved, that 
when we look at Sirius, the rays which enter the eye cannot 
have been less than 6 years and 4^ months coming from that 
star to the observer. Hence it follows, that when we see an 
object of the calculated distance at which one of these very 
remote nebulae may still be perceived, the rays of light which 
convey its image to the eye, must have been more than nine- 
teen hundred and ten thousand, that is, almost two millions of 
years on their way ; and that, consequently, so many years ago, 

* See Phil. Trans, for 1800, page 83. N. B. In the same page, line zz, for 5000 
read 50000. 



of 500 new Nebula, and Clusters of Stars, 499 

this object must already have had an existence in the sidereal 
heavens, in order to send out those rays by which we now 
perceive it. 

VIII. Of Stars with Burs, or Stellar Nebula. 

Situated as we are, at an immense distance from the remote 
parts of the heavens, it is not in, the power of telescopes to 
resolve many phenomena we can but just perceive^ which, could 
we have a nearer view of them, might probably shew them- 
selves as objects that have long been known to us. A stellar 
nebula, perhaps, may be a real cluster of stars, the whole light of 
which is gathered so nearly into one point, as to leave but just 
enough of the light of the cluster visible to produce the appear- 
ance of burs. This, however, admits of a doubt. 

IX. Of milky Nebulosity. 

The phenomenon of milky nebulosity is certainly of a most 
interesting nature : it is probably of two different kinds ; one of 
them being deceptive, namely, such as arises from widely ex- 
tended regions of closely connected clustering stars, contiguous 
to each other, like the collections that construct our milky-way. 
The other, on the contrary, being real, and possibly at no very 
great distance from us. The changes I have observed in the 
great milky nebulosity of Orion, 23 years ago, and which have 
also been noticed by other astronomers, cannot permit us to 
look upon this phenomenon as arising from immensely distant 
regions of fixed stars. Even Huygens, the discoverer of it, 
was already of opinion that, in viewing it, we saw, as it were, 
through an opening into a region of light * Much more would 

* See Systema Saturnium, page 8 and 9. 



#oo Dr. Herschei/s Catalogue 

he be convinced now, when changes in its shape and lustre have 
been seen, that its light is not, like that of the milky-way, com- 
posed of stars. To attempt even a guess at what this light may 
be, would be presumptuous. If it should be surmised, for in- 
stance, that this nebulosity is of the nature of the zodiacal 
light, we should then be obliged to admit the existence of an 
effect without its cause. An idea of its phosphorical condition, is 
not more philosophical, unless we could shew from what source 
of phosphorical matter, sUch immeasurable tracts of luminous 
phenomena could draw their existence, and permanency ; for, 
though minute changes have been observed, yet a general re- 
semblance, allowing for the difference of telescopes, is still to be 
perceived in the great nebulosity of Orion, even since the time 
of its first discovery. 

X. Of nebulous Stars. 

The nature of these remarkable objects is enveloped in much 
obscurity. It will probably require ages of observations, before 
we can be enabled to form a proper estimate of their condition. 
That stars should have visible atmospheres, of such an extent 
as those of which I have given the situation in this and my 
former catalogues, is truly surprising, unless we attribute to 
such atmospheres, the quality of self-luminous milky nebulosity. 
We can have no reason to doubt of the starry nature of the 
central point ; for, in no respect whatever does its appearance 
differ from that of a star of an equal magnitude ; but, when the 
great distance of such stars is taken into consideration, the real 
extent of the surrounding nebulosity is truly wonderful. A very 
curious one of this kind will be found in the 4th class, No. 6q, 
of the annexed catalogue. 



of 500 new Nebula, and Clusters of Stars. 501 

XL Planetary Nebula. 

This seems to be a species of bodies that demands a particu- 
lar attention. To investigate the planetary nature of these 
nebulas, is not an easy undertaking. If we admit them to con- 
tain a great mass of matter, such as that of which our sun is 
composed, and that they are, like the sun, surrounded by dense 
luminous clouds, it appears evidently that the intrinsic bright- 
ness of these clouds must be far inferior to those of the sun. A 
part of the sun's disk, equal to a circle of 15" in diameter, would 
far exceed the greatest lustre of the full moon ; whereas, the 
light of a planetary nebula, of an equal size, is hardly equal to 
that of a star of the 8th or 9th magnitude. If, on the other 
hand, we should suppose them to be groups, or clusters of stars, 
at a distance sufficiently great to reduce them to so small an 
apparent diameter, we shall be at a loss to account for their 
uniform light, if clusters ; or for their circular forms, if mere 
groups of stars. 

Perhaps they may be rather allied to nebulous stars. For, 
should the planetary nebula? with lucid centres, of which the 
next article will give an account, be an intermediate step be- 
tween planetary nebulas and nebulous stars, the appearances of 
these different species, when all the individuals of them are fully 
examined, might throw a considerable light upon the subject. 

XII. Of planetary Nebula with Centres. 

In my second catalogue of nebulas, a single instance of a 
planetai-y nebula with a bright central point was mentioned; 
and, in the annexed one, No. 73 of the 4th class, is another of 
very nearly the same diameter, which has also a lucid, though 

mdcccii. 3T 



£oa Dr. Herschei/s Catalogue 

not quite so regular a centre. From several particularities 
observed in their construction, it would seem as if they were 
related to nebulous stars. If we might suppose that a gradual 
condensation of the nebulosity about a nebulous star could take 
place, this would be one of them, in a very advanced state of 
compression. A further discussion of this point, however, must 
be reserved to a future opportunity. 



CORRECTION OF A FORMER PAPER. 

In my Paper on two lately discovered celestial Bodies, 
Page 224, line 18, of this volume, instead of 135, read -31. 



oj 500 new Nebula, and Clusters of Stars, 



$°S 



Catalogue of 500 additional new Nebula, and 
Clusters of Stars. 



First Class. Bright Nebula. 



I. 


1788. 


Stars. 




M. 


s. 




D. M. % 


i Description. 


216 


Dec. 3 


22 Ursge 


P 


13 


5* 


/ 


3 4 s 


s ^B.^L.z'F.r.w^M. Towards 
the ff within the nebulo- 
sity, is a f S. /£. 


217 


27 


54 Persei 


f 


9 


25 


n 


46 s 


5 cB. cL. mbM. Stands nearly 
in the center of a trape- 
zium. 


218 


Si 

1789 


63 Auriga* 


f 


2,6 


43 


I 


O 20 1 


cB. R. vgmbM. about %'d. 


219 


Mar. 23 


55 Ursa? 


I 


5 


33 


n 


O 361 


vB. cL. iF. vgmbM. 


220 


Apr. 12 


64 (q/) Ursas 


P 


43 


.59 


J 


20 S 


1 cB. mE. 70 np ff. 3 or 4' /,■ 


221 


_ 


— — 


P 


21 


4 1 


I 


O 37 s 


j cB. R. vgmbM, 4 or 5'^. 


222 


_ 


— — 


P 


20 


20 


I 


35 s 


i cB. z'E. near mer. g&M. 2'/. 


223 


— 


— — 


I 


6 


4 


I 


2 45s 


i z>B. mE. »/> ^: BN. 5'/. ii'6. 


224 


— 


1 Canum 


P 


9 


13 


I 


3 10s 


JcB.^L.mE. SN. 


225 


— 


— — 


P 


8 


3i 


I 


46j£ 


t i>B. pL. BrN. just/ a r/5f. 


226 


14 


64 [y) Ursse 


P 


33 


32 


I 


34' 1 


cB.R.SBrNandrFchev. tfd. 


227 




— ^ — 


P 


15 


28 


n 


3 37| s 


1 cB. cL. iF. r. vgbM. g'l. v'b. 


228 


— 


— — 


P 


5 


20 


n. 


2 24s 


1 vB. vBiN. and F. bran. i±'h 
i'b. 
The 2d of 2. vB. R. vgbM. 


229 


_ 


_ __ 


f 


3 


46 


n 


i 47 3 


















See II. 791. 


230 


— — 


83 Ursee 


f 


20 


24 


n 


27 s 


>.cB. S. E.y/> «/. cBN. and F 
bran. 


231 


— 


— — 


f 


24 


34 


n 


10s 


s cB. />S. iR. 


232 


■ " 


■ " ' ' " 


f 


27 


7 


n 


16 j 


The adofa.cB.S.R.tg-m&M. 
See III. 791. 


233 


V7 


44 Ursee 


I 


1 


14 


I 


16 s 


i cB. E. 30°^ nf.r. mbM. 3'/., 



3 T 2 



504< 



Dr. .Herschei/s Catalogue 



I. 


1789. 


Stars. 




M. 


s. 




M. D 


£ Description. 


234 


Apr. 1 7 


74 Ursae 


/ 


1 


31 


/ 


O 28' 


2 cB. S. /E. Just^> a phft. 


235 


— 


12 (-*) Draconis 


P 


66 


52 


/ 


2 3<. 


1 cB. iF vgmbM. 7' /, 5' b. 


236 


— 


— __ 


P 


59 


56 


I 


2 13. 


$vB. S. z'R. Bz'rN. vgmbM. 


237 


— 


_ ' — 


P 


54 


10 


/ 


O 52 


1 B. z oval. vgmbM. 


238 


24 


69 Ursae Hev. 


I 


27 


55 


/ 


32$ 


1 cB. ph. iR vgmbM. 


239 


— 


— — 


f 


28 


10 


/ 


17gcB.pL. E.mbM. 


240 


— 


— — 


J 


28 


34 


/ 


ty^cB.pL.E.SBN. 




1790 
















241 


Feb. 17 


19(g) Hyd.Crat. 


P 


H 


43 


/ 


57 1 


l cB. E. 70 «/>^f. vgbM 7'/, 
4'6. within a parallelo- 
gram. 


242 


Mar. 17 


15 (/) Ursae 


P 


15 


4° 


/ 


21 1 


vB. LBrN. with vF chev. 


243 


— 


77 (e) Ursa? 


I 


1 


47 


n 


2 251 


1 cB. S. R. gbM. 


244 


18 


39 Ursae 


f 


36 


44 


n 


40 s 


.cB.R. vgmbM. i±'d. 


®45 


— 


— — 


I 


39 


27 


n 


1 58£ 


> vB. cL. R. vgbM. 


246 


— 


66 Ursae - 


P 


29 


19 


n 


20 s 


.cB.ph.E. 


247 


__ 


— — 


P 


28 


*3 


n 


2 OS 


1 vB.pL. IE. near par. mbM. 


248 


— 


— — 


P 


7 


5 


n 


2 52 s 


uB.p'L.iF. 


249 


19 


1 7 Ursae 


P 


9 





n 


3 43 s 


> cB E. near par. er. bM. 4' /, 
2' 6. I suppose, with at 
higher power and longer 
attention, the stars would 
become visible. 


250 


— 


— _ 


P 


4 


47 


n 


3 17 ] 


1 vB. cL. IE. LBNM. 


251 


, 


76 Ursae 


P 


50 


48 


I 


2 31 


vB. perfectly R. BN and F 
chev. vgbM. \\' d. 


252 


— 


_ — 


P 


41 


ji 


I 


34 1 


vB. cL. R. 


253 


— 


— — 


P 


41 


46 


J 


51 1 


vB. vh. E. 


254 






P 


1 


47 


I 


1 81 


eB. E. par. 5' I. all over 
equally B. except just on 
the edges. 


255 


— 


69 Ursae Hev. 


f 


19 


26 


n 


1 1 1 


vB, BENM. 3' /. \> b. 


256 


— 


— . — 


I 


21 


33 


n 


13] 


vB.ph. iF. suddenly mbM. 


257 


Oct. 9 


12 Eridani 


I 


16 


58 


I 


1 581 


cB. iR vgmbM. i±'d. 


258 


Dec. 28 


47 (a) Persei 


P 


3 


41 


n 


1 O] 


vB.iF.r.bM.s'l.^'b.ApL 
star in it towards the f 


















side, but unconnected. 



of 500 new Nebula, and Clusters of Stars. 



505 



I. 


1791. 


Stars. 




M. 


s. 




D. M. « 


1 Description. 


259 


Mar. 7 


17 Hydras Crat. 


/ 


18 


3 1 


ra 


O 27] 


cB.p~LJE.gbM. Thebright- 
ness takes up a large space 
of it. 


260 


Apr. 2 
*793 


23 (b) Ursa? 


P 


1 


49 


/ 


34' 


vB. vS, iR. mbM. 


261 


Feb. 4 


38 of the Connois. 


f 


3 


7 


/ 


1 35i 


vB. iR. vgbM. s'd. Seems 
to have 1 or 2 stars in 
the middle, or an z'N ; the 
chev. diminishes vg. 


262 


Apr. 6 


1 (x) Draconis 


P 


2 


6 


/ 


2 41 1 


cB. vS. iF. N. with vF. chev. 


263 


— 


4 Draconis - 


P 


22 


48 


J 


231 


cB. IE. bM. 


264 


7 


— — 


P 


*4 


18 


n 


1 36*1 


cB. S. 6M. 


265 


8 


37 Ursse 


P 


16' 


16 


n 


1 51 


cB. S. /R. vgmbM. 


266 


— - . 


— — 


P 


13 


35 


J 


11 1 


cB. ph. iF. gbM. 


267 




39 Ursse 


f 


11 


21 


I 


10 1 


cB.ph. iR. i±'d.. The great- 
est part of it almost e- 
qually B. 


268 


— 


— — 


f 


12 


46 


f 


41 


vB. vS. R. Stellar. 


2% 


— 


— — 


f 


18 


1 


n 


29 1 


cB. R. 1 'd. just n of a Sft. 


270 


— . 


_ — 1 


f 


35 


2,6 


n 


1 42 s 


s vB. ch. E. par. SN. E par. 


271 


— 


— — 


f 


35 54 


n 


551 


. v B. ch. E. mbM. 




1796 
















272 


Mar. 4 


Georgian planet 


P 





53 


n 


6 s 


icB.S.iR. BN.mbM. This 
nebula was seen at g h 27', 
sidereal time; the tele- 
scope being out of the 
meridian. 


373 


Nov. 22 


A double star 


f 


. 5 45 


I 


891 


) vB. vh. E. near par. The 


















determining star follows 


















5DraconisHevelii 13' 54" 
in time, and is o° 23' more 
south. 


274 


— 


'__ _ — 


I 


10 


13 


I 


24? 


j cB. vS. *R, bM. 


275 


Dee. 10 


5 Dracon. Hev. 


f 


1 


32 


11 


12s 


1 cB. S. R. 


276' 


— 


_ _ — 


f 


2 


45 


n 


12s 


1 cB. ch. iF. IE. mbM. 


277 


— 


— — 


J 


6 


20 


n 


O 20 5 


1 vB. ch. IE. mbM. 


278 


12 


— — 


P 


11 


5 


J 


O 15^ 


icB.ch.iR. mbM. 



§oS 




Dr. 


H 


ERSCHEI 


's 


Catalogue 


i. 


1796. 


Stars. 




M. S. 




D. M.J 


> Description. 


®79 


Dec. 12 


— — - — — 


P 


IO 28 


n 


1 38 2 


cB. cL. /E. 6M. 


280 


1798 


i6(£)Ursa2min. 


f 


51 33 


n 


$i 


• »B. dL. /E. #>M. The great- 
est brightnes confined to 


281 


Dec. 9 


t Apps. Sculps. 








! 


a small noint. 






L.C.95 - 


P 


1 47 


n 


O 27 1 


cB. E. np ff. NM. Q'l. i%h. 




1801 














282 


Apr. 2 


2o8(N)Camelop. 
















of Bode's Cat. 


P 


i53 15 


1 


2 43 1 


cB. ph. z'F. 


283 


— 


— — 


P 


113 40 


1 


3 4 1 


cB. cL. er. 


284 


— 


. -»_ — 


P 


85 18 


J 


23 5 


cB. pS. z'F. 


285 


Nov. 8 


24 (d) Ursas 


J 


13 14 


J 


1 53 5 


vB. vL. E. a^. 6'/. Q'b. 


286 






f 


3° ° 


J 


1 8i 


. vB. cL. R. vgmbM. On the 
north-following side there 
is a F ray interrupting the 
roundness. 


287 


Dec. 7 
1802 


1 (a) Draconis 


P 


4 37 


n 


1 131 


cB. mE. np Jf. mbM. 3'/, l'b. 


288 


Sept. 26 


184 Camelopar. 










* 




J of Bode's Cat. 


P 


n 58 


J 


2 34 


1 vB. cL. IE. suddenly mhM. 


Second Class. Faint Nebula. 


11. 


1789. 


Stars. 




M. S. 




D. M. ; 


r Description. 


7% 


Feb. 22 


81 [g) Geminor. 


P 


37 58 


n 


O 4 


1 pB. pL. iR. er. bM. 


770 


— 


62 Ursaa 


P 


13 44 


J 


2 15- 


1 pB. pL. R. IbM. 


771 


Mar. 20 


2 ^'(%) Virginis 


P 


7 


n 


O 26'! 


2 pB. cL. z'F. *r. w6M. 4 or 5'd. 


772 


— 


— — 


f 


3 9 


n 


57- 


i F. S. E. 


773 


— 


— — 


f 


3 5 


n 


1 i ; 


2 F. S. E. bM. 


774 


"""■" 


— _ 


f 


6 27 


n 


55 c < 


i pB. S. iR. mbM, 


775 


23 


55 Ursse - 


f 


3 S.i 


J 


25- 


i pB. cL. IE. vgmbM. 


776 




26 (%) Virginis 


P 


8 19 


J 


4 


1 F. pL. er. 


777 


• __ 


— . — 


I 


17 ] 5 


n 


1 9' 


t F. S. R. 6M. 


778 




— — 


f 


21 12 


n 


1 54 


i F. S. //". a double star. 


779 




16 (%) Virginis 


f 


22 44 


n 


14 


1 F. S. 


780 


26 


46 ( 7 ) Hydrae 


f 


1 22 


I 


1 14J 


1 F. R. r. vglbM. 4V. 



of goo new 'Nebula, and Cluster* of Stars. 



507 



II. 


1789. 


Stars. 




M. S. 




D. M. 


y Description. 


781 


Apr. 12 


1 Canura - 


P 


10 55 


/ 


53' 


2 ApS.ft. involved in nebu- 
losity of no great extent ; 
theft, does not seem to 
belong to it. 


782 


H 


64 (y) Ursas 


P 


31 7 


n 


7 


1 pB. S. R. vgmbM. just fa 
Sft. 


783 


— 


— — 


P 


18 40 


n 


50 


i pB. ph. bM. 


784 


— 


— i — 


P 


17 4» 


n 


37 • 


1 pB. ch. IE. 2>'l 


785 


— 


— - _— 


P 


7 3 


n 


2 18: 


ipB. S.-/E. 


786 


— 


— — 


P 


3 31 


n 


1 39 


F. E. 


787 


}- 




P 


3 2 


W 


1 27. 


r Two nebulae; the ist^B. S. 
l lThe2d^B. S. 


788 




3 7 


it 


1 24 


789 

790 


}- 


— — 


I 


1 25 


n 


1 38: 


r Two nebulas; the 1 stpB. E. 
1 1 The 2d F. S. 


791 


— 


, __ . — 


f 


3 3 4 


n 


1 483 


i The 1st of 2. pB.S.E. See 
I. 229. 


792 


— 


1 Canum - 


P 


3 12 


n 


3 47" 


t F. S. R. bM, 


793 


— 


— _ 


P 


57 


n 


2 365 


1 F. pL. i¥. bM. 


794 


— 


77 (e) Ursa? 


P 


11 32 


J 


49 s 


1 F. S. 


795 


— 


— — - 


P 


8 25 


J 


1 13 s 


j j&B. v S. m&M. 


796 


— 


— ■ _. 


P 


7 20 


I 


1 25 s 


j />B. cS. /E. BrN. 


797 


— 


8 1 Ursas 


P 


3 33 


f 


2 18s 


j />F. pS. R. t^M. 


798 


— 


83 Ursas - 


J 


49 


n 


111 


/>B. E. ii'/, f6. 


799 


— 


— — 


f 


21 27 


n 


1 7 s 


j />B. cL. E. 


800 


— 


. . — ■ — 


I 


25 7 


n 


1 2 ] 


1 pB. S. 


80 1 


— 


— . _. ■ 


1 


27 27 


n 


23 s 


5 F. cL. 


802 


17 


71 Ursas - 


P 


15 20 


n 


1 331 


F. S. E. 


803 




— — 


P 


*3 57 


n 


59 s 


s F. S. R. 


804 


— 


— — 


P 


5 43 


J 


31 


/>B. />L. z'F. 


805 


— • 


— • — 


P 


4 41 


n 


1 201 


The 2d of 2./>B./>L. w6M. 
See III. 798. 


806 


— 


— _. 


P 


2 13 


n 


1 42 J 


/>B. 


807 


— 


i2(<) Draconis 


P 


55 48 


n 


42 1 


/>B. E. mer. \\'l, |6. 


808 


24 


Neb. II. 756 


P 


24 16 


n 


41 i 


1 />B. S. z'F. er. mixed with 
some/>L. stars, which may 
perhaps belong to it, 


809 


"™* 


- — — _ ■ 


P 


15 5 


J 


263 


F. S. E. 



5 o8 



Dr. Herschei/s Catalogue 



II. 


1789. 


Stars. 


P 


M. S. 




D. M 





Description. 


8io 


Apr. 24 


21 ([a.) Draconis 


4 6> 3i 


n 


3 3 3 


1 


/>F. pS. IE. 


811 


— 


— — 


P 


44 9 


n 


50 


1 


pB. z'R. vgvlbM. 


812 


- — 


- — — 


I 


10 4 


n 


2 55 


1 


F. S. R. ^/6M. 


813 


26 


5 Canum 


P 


10 53 


I 


50 


1 


/>B. S. IE. 


814 


- — 


7 Canum 


I 


20 24 


n 


1 20 


1 


F. S. tj/k6M. 


815 


— 


82 Ursa? 


P 


3 1 48 


I 


52 


1 


F.t>S. Stellar. 


816 


— 


— . — 


P 


9.6 52 


J 


1 36 


1 


F. S. zR. vgmbM. 


817 


— 


— — 


P 


3 4 2 


I 


1.4° 


1 


pB. S. R. ^6M. 


818 


1790 


12 Draconis 


P 


40 16' 


n 


33 


1 


pY. c$. R. i>#6M. 


819 


Mar. 8 


ig{x)Hyd.Crat. 


P 


11 58 


n 


31 


1 


/>F./L. iF. bM. 


820 


10 


65 Auriga? 


f 


7 22 


n 


1 


1 


pB. S. Stellar. 


821 


— 


7oGeminorum 


P 


1 43 


n 


12 


1 


pB. cS. r. p a eft. 


822 


n 


27 Lyncis - 


P 


25 42 


n 


41 


1 


pY. R. r. vgbM. 


823 




15 (I) Ursas 


P 


12 10 


J 


18 


1 


pB. S. R. w&M. 


824 


— 


26 Ursae - 


f 


*39 17 


J 


1 


1 


/>B. mE. 67, 2'6. 


825 


_ 


— — 


J 


139 40 


J 


1 44 


1 


/>B. S. fF, 6M. 


826 


— 


77 (s) Ursas 


f 


28 


n 


1 42 


1 


F. S. E. 


827 


— 


— — 


I 


69 59 


n 


3 27 


1 


pB. S. z'F. mbM. 


828 


18 


17 Ursaa 


P 


6 25 


J 


2 57 


1 


pB. S. vgmbM. 


829 


— 


66 Ursa? 


P 


3i 14 


n 


1 9 


2 


Y.E.npff.er.ii'l. 


830 


— 


— — . 


P 


15 23 


I 


20 


1 


pB. E. 


831 


— 


— — 


P 


11 44 


n 


1 22 


1 


/>B. r;S. IE. 


832 






P 


6 53 


u 


2 52 


2 


pB.pL. R. The nebulosity 
of this runs into that of 
I. 248. 


833 


— 


. : 


P 


1 1 


n 


1 4 6 


1 


F. S. 


834 


19 


17 Ursaa 


P 


11 34 


n 


3 10 


1 


pY. pS. iY. er. 


835 


— 


29 (u) Ursa? 


J 


5 " 


n 


15 


2 


F. S. E. near par. 


836" 


— 


76 Ursaa 


P 


70 41 


I 


53 


1 


F. S. R. r. almost of equal 
light throughout. 


837 


— 


— . — 


P 


66 54 


J 


1 


1 


pB. IE. 


838 


— 


— — 


P 


66 15 


J 


3 9 


1 


pB. S. 


839 


— 


— — 


P 


63 


J 


2 28 


1 


pB. cS. R. mbM. 


840 


— 


— . — _ 


P 


47 3o 


J 


2 16 


1 


Y. S. bM. 


841 


— 


69 Ursas Hev. 


I 


4 24 


n 


2 46 


2 


The 1st of 2. pB. S. iY. 


842 


— 


— — 


J 


4 35 


n 


2 50 


2 


The 2d of ^. pB.pl,. iY. 



of 500 new Nebula, and Clusters of Stars. 



509 



II. 


1790. 


Stars. 




M. S. 




D. M. 

42 


Description. 


843 


Mar. 19 


__ _ _ 


/ 


26 40 


n 


iF. S. 


844 


— . 


— . — 


J 


2 7 43 


I 


29 


1 pB. cL. 


845 


20 


50 («) Ursae 


/ 


22 41 


n 


1 44 


3 pB.pL. z'R. bM. 


846 


— 


76 Ursas - 


P 


23 9 


n 


3 13 


1 pB. mE.fpnf. BN. gl,±'b. 


847 




— — 


P 


19 1 


n 


3 8 


1 pB. S. IE. 


848 


— 


— — 


P 


14 Q i 


n 


2 8 


1 F. iF. bM. Stellar. 


849 


— 


— — 


P 


9 7 


n 


1 15 


1 pB. vS. IE. SN. 


850 


— 


— , — 


P 


7 16 


n 


48 


1 pB. ph. iR. r. vgbM. 


851 


Oct. 9 


72 Pegasi 


I 


18 3 


I 


6 


2 pF.ph. iR. IbM.fp.avSft, 


852 


— 


o- Fornacis L. C. 
















285 - - 


P 


4 *5 


I 


34 


iF.ph.iR.gbM. 


853 


Nov. 26,29 (tt) Androm. 


P 


25 3 8 


J 


24 


1 F. S. E. nearmer. 


854 


Dec. 25 


44 Piscium - 


f 


3 49 


n 


56 


1 pB. vS. R. vgmbM. pretty 
well defined on the mar- 


855 


— ; 


— — 


I 


4 44 


n 


10 


gin. 
2 pB. ch. iR. r. vgbM. fp. a 
vSJt. 


856 


— 


— — 


f 


13 52 


n 


1 8 


1 F. S. vgbM. 


857 


— 


— — 


J 


13 52 


n 


53 


1 F. S. vgbM. 


858 


— 


— — 


f 


14 10 


n 


58 


1 pB. S. vgbM. 


859 


— 


98 (jt*) Piscium 


I 


20 28 


n 


1 


1 pB S. E. near par.^fr. a S/£. 


860 


28 


Mayer's Zod. 
















Cat. No. 18 


P 


5 4 8 


n 


39 


1 pF. vS. vgbM. 


861 


— 


57 Auriga? - 


J 


17 30 


n 


1 54 


1 pB. ph. iF. gbM. 


862 


— 


— ' — 


f 


23 5 


n 


1 29 


iF.pL. 


863 


2 .9 


63 ($) Piscium 


P 


39 


n 


44 


1 ph. IE. r. gbM. 


864'Mar. 7 


17 Hyd. Crat. 


f 


16 46 


s 


1 


1 pB, S. R. vgmbM. almost 
















resembling a N. 


8% 
866 














r Two nebulas, both F. S. R. 


}- 


— — - 


f 


34 2 


J 


3 1 


1 1 bM. and nearly in the 
















[ same par. 


867 


April 2 


73 Ursa? 


P 


14 8 


I 


1 12 


1 pB. vS. Stellar. 


868 








10 38 

11 8 






r Two nebulse, the 1st F. S. 


86 9 


} 8 


14 (t) Ursae 


f 


n 


47 


1 iF. 


J 




J 






[The2dF.*L.E. 

1 



MDCCCII, 



3 U 



£10 



Dr. Herschei/s Catalogue 



ii. 



870 



April 3 



874 
875 



1791. 



35 Ursa? - 



871 
872 

873 May 6 



Stars. 



3 
1792 

876 Apr. 20 22 (f) Bootis 

877 - _ _ 

878 Sept 16 3CepheiHev. 



1753 
879 April 6 

880 
881 



3 (yjUrsasmin. 
24 37 (I) Bootis 
;o 25 Herculis 



7 

882 8 

883 

884 

885 

886 

887 

888 

889 May 1 2 

890 

891 

892 

893 
894 

895 

896 

897 



898 



1 (a) Draconis p 
P 



4 Draconis 
37 Ursa? 

39 Ursa? 



942 Ursa? 
19 Bootis Hev. 



/ 

/ 
/ 
/ 
/ 
/ 

P 

P 



i393( T )Virginis 

Sept. 6 53 Aquarii 

1794 

Georgian planet 



P 
f 
I 

J 
I 
I 
P 
P 
I 
I 
I 
I 
P 
P 



J 



M. S. 



2 50 

3 37 

21 gO 

37 53 
34 4 8 

3 10 

1.5 58 

13 27 

29 1 5 
9 49 



/ 

/ 

n 

I 

I 

n 

n 
n 

I 
I 



D. M. 



7 44 M 



45 43 n 



o 12 



10 40 

8 36 

22 42 

37 41 

44 5 

2 41 
7 21 

26 45 

13 20 

6* 44 

7 44 

9 37 
10 46* 

21 54 
21 49 
16 29 

3 ° 



n 
n 

I 
n 

I 
n 

n 

11 

n 

n 

n 

\ 

n 

n 



o 3 6 

o 52 

11 

1 17 

1 12 

2 12 

26 

1 21 

o 25 



3 

8 

37 

42 
2 

56 
11 

20 

33 

8 

24 
22 

31 

40 

40 
7i 



Description. 



F. S. iR. Almost of equal 

light throughout. 
F. vS. mbM. 
F. cL. iR. 
F. R. 6M. i'd. 
pB.ph. iR. vgmbM, 
pB.S. IE. vgmbM. 



o 33 



vS. 
pB. ph. iF. 
pB. iF.bM. contains 2 stars. 

pB. S. R. bM. 

F. S. /E. fp nf. but near 

mer. gbM. 
F. wE. «/>^. but near par. 

if/. 
pB.pL.lE.bM. 
F. S. R. bM. 
F. S. R. 6M . 
F. S. /E. w/)^. 
/>B. iF. 

F./>L. /F. bM. 
F. S. R. 6M. 

pB. pL. R. just foil, a S/t 
/>B. />L. z'R. 
pB. ph. IE. BM. 
F. S. E. near mer. 
pB. S. iF. 
F. S. 
F. S. iR. 
F. S. ?R. 
^B. IE. r. if/, if 6. 

F. 3' north of a />L. red ft. 
This nebula was seen at 
8 h 49', sidereal time, the 



of goo new Nebula, and Clusters of Stars. 



£11 



II. 


1797. 


Stars. 


— 


M. S. 




D. M. 




a* 


Description. 
















telescope being out of the 


















meridian. 


$99 


Dec. 20 
1798 


4t(b) Urseemin. 


P 


26 13 


/ 


40 


1 


F. S. E, near mer. i'I. 


9 00 


Dec. 10 
1799 


18 (e) Eridani 


P 


20 53 


y 


1 5 


1 


F. E.fp nf. near par. 3'/, x'b. 


901 


June 29 


93 Herculis - 


P 


2:7 30 


/■ 


11 


1 


F. S. i¥. er. 2'/. 


902 


1801 


— . — 


I 


7 47 


n 


49 


1 


F.^L. R. vgbM.^'d: 


9°3 


April 2 


2o8(N)Camelop. 


















of Bode's Cat. 


P 


139 19 


f 


1 39 


1 


F. pL. r. 


904 


— 


— — 


P 


6"8 9 


1 


1 5 8 


1 


F. pL. IbM. 


905 


— 


. _*_ — 


P 


3 6 53 


! 


2 22 


1 


pB. ph. 


gob 


Nov.28 
1802 


11 (a)Draconis 


I 


86 13 


n 


8 


1 


F. 8. lE.fpnf.vglbM. 


907 


June 26 


2 (p) Lyraa 


f 


5 21 


n 


18 


1 


F. S. *F. 



jfi6z'rd C/ass. Very faint Nebula. 



III. 


1788. 


Stars. 




M. S. 




D. M. 





Description. 


748 


Dec. 3 


43 Camelop. 


/ 


35 5 


w 


29 


1 


»F. z>S. has a vF. bran «/. 


749 


. — 


22 Ursas 


/> 


12 45 


./' 


24 


1 


6-F. z>S. 


75^ 


3i 


63 Auriga? - 


./ 


48 58 


re 


4,3 


i 


vF. S. R. /6M. 


75i 


1789 


39 Lyncis - 


/ 


25 15 


y 


30 


2 


*F. S. 


752 


Feb. 22 


16 (£") Cancri 


P 


4 19 


n 


8 


1 


eF, IE. f of sl v$ft. 


753 


— 


33 ( r ) Cancri 


P 


8 11 


1 


4 


1 


vF. S. R. v/&M. 


754 


24 


6 Corvi 


P 


17 33 


/ 


1 43 


1 


^F. wS. R. 


755 
756 


"iMar. 
J 2 ° 














f Two nebulae, both t>F. vS. 


26 (%) Virginis 


P 


13 3 


» 


so 


1 


•j E. within if of each 
I other. 


757 


- 




P 


5 25 


n 


38 


2 


2 vS. stars involved in »F. 
nebulosity of no great ex- 
tent. 



3U 2 



513 



Dr. Herschei/s Catalogue 



III. 


1789. 


Stars. 




M. S. 




D. M. < 


3 Description. 


758 

759 


->Mar. 
J 23 


— . — 


/ 


SO 55 


n 


1 53 


1 Two nebulas, both vF. vS. 


760 


— 


_ __ 


/ 


23 47 


I 


9 


1 cF. vS. R. 


761 


— 


— — 


/ 


24 55 


n 


18. 


1 vF. S. 


762 


— 


102 (u')Virginis 


P 


11 30 


n 


36 


1 vF. vS. 


7^3 


— 


10 5(<p) Virginis 


P 


1 1 


I 


1 


t eF. S. 


7^4 


26 


9 (0) Corvi 


P 


4 55 


n 


15 ■ 


1 cF. pS. R. Stellar. 


765 


— 


45 (40 Hydra 


P 


1 35 


I 


53 


ivF.pL. z'F. 


766 


___ 


— _ 


J 


39 


I 


16' ■ 


1 i>F. » S. 


767 


Apr. 12 


64 (y) Ursse 


P 


78 24 


J 


3 45i 


i vF. p$. i E. 


768 


— 


— — 


P 


30 48 


J 


49 s 


$z>F. vS. Stellar. 


769 


— 


— — 


P 


1 40 


I 


1 44] 


t cF. S. 


77o 


14 


—— .— — .- 


P 


39 3 2 


n 


2 2 : 


1 vF. vS. Stellar. 


77i 






P 


19 37 


n 


1 8 


i<?F. S. z'E On account of 
the brightness of 1 yg Ur- 
sae maj. of Bode's Cat. 
which was in the field of 
view with it, I had near- 
















ly overlooked it. 


772 


— . 


__ . — . 


P 


19 2 


n 


1 16 ] 


.vF. Stellar. 


773 


— 


— — 


P 


14 


n 


2 32 1 


uF.pS. ZE. just/ a vS/f. 


774 


— 


— ■ — 


P 


10 37 


f 


58 s 


svF. S. 


775 


— 


__ — 


P 


10 17 


I 


1 1 ] 


1 vF. vS. 


776 


— 


. — __ 


P 


9 33 


n 


2 12 ] 


1 eF. pL. IF. 


777 


, — . 


1 Canum - 


P 


1 54 


/ 


331 


ieF. S. Stellar. 


778 


— ■ , 


77 (e) Ursas 


t 


9 10 


i 


1 4s 


icF.S.lE.iF. 


779 


— , 


— __ 


f 


11 36 


n 


20 s 


*t>F. S. 


780 


— . 


— __ 


I 


12 37 


I 


19] 


1 cF. S. 


781 

782 


}- 


— , __ 


J 


12 30 
12 44 


I 


2 22 

2 20 ' 


t j Two nebulae. Both vF. S. 


7 8 3 


— 


— . — 


I 


12 33 


J 


2 28 : 


1 vF. S. E. 


784 


— 


81 Ursaa 


P 


7 6 


n 


9 


1 cF. S. zR. 


785 


— 


83 Ursas 


I 


4 34 


n 


37 


1 2 <?F. ft. with nebulosity. 


786 


__ 


— , — , 


f 


14 3 


J 


22 


lfF.f'S. Stellar. 


787 


— 


— . — 


I 


22 27 


J 


28 


1 vF. vS. 


788 


. — 


— , __ 


f 


23 47 


I 


24 


1 f F. vS. 


789 


" 


ft*™* 1 .mi .1 1, 


f 


23 54 


I 


22 


1 vF. vS. 



of 500 new Nebula, and Clusters of Stars. 



5*3 



III. 


1789. 


Stars. 




M. S. 




D. M. 5 


r Description. 


790 


Apr. 14 


83 Ursse 


/ 


25 23 


/ 


O 171 


vF. pL. 


791 


— 




/ 


27 7 


n 


O 16 1 


l The 1st of 2. vF. S. 4'dist. 
from I. 232. 


7.92 


17 


44 Ursse 


P 


2 11 


n 


50 ] 


v F. S. E. 20°^5> nf. er. 


793 




48 (jG) Ursse 


I 


1 25 


I 


O IOI 


vF. vS. Stellar. The bright- 
ness of jS Ursse is so con- 
siderable, that it requires 
much attention to perceive 
this nebula. 


794 


— 


71 Ursse 


P 


22 30 


n 


1 8i 


cF. S. ver30o» 


795 


— 


— — 


P 


16 8 


n 


2 52 


, vF. S. iF. r« 


796 


— 


— — 


P 


11 23 


n 


2 52 J 


eF. 


797 


— 


_ — 


P 

P 


10 56 


n 


3 11S 


s vF. S. 


798 


— 


_ — . 


5 4 


n 


1 20] 


1 The 1st of 2. cF. IE. iF. II. 








X 








805. 


799 


, — 


— . — 


P 
P 


1 12 


n 


1 361 


1 t>F. v S. 


800 
801 


}- 


— — 


1 9 


n 


I 371 


r Two nebulse, both eF. cS„ 
1 I R. 


802 


___ 


74 Ursas 


f 


4 54 


n 


O 3OS 


j The 1st of 2. vF. S. /E. See 














III. 807. 


803 


— 


69 Ursse Hev. 


f 


9 33 


I 


2 53 c - 


j eF. fS. 


804 


— 


— — 


J 


46 59 


I 


2 18s 


s eF. S. E. r. 


8o 5 


— 


— — , 


f 


48 9 


I 


1 1 


5 eF. vS. R. Stellar. 


806 


— 


i2(<) Draconis 


J 

P 


34 20 


n 


8i 


1 1> F. z> S. IF. 


807 


24 


74 Ursse 


I 


5 26 


n 


34 


1 The 2d of 2. eF. S. E. diffe- 
rently from III. 802. 


808 


— 


69 Ursse Hev. 


P 


7 35 


I 


2 19] 


1 cF. S. E. 


809 


— 


— — 


f 


27 7 


I 


1 25] 


1 vF. vS. 


810 


— 


— — 


I 


30 44 


f 


13 


1 cF. vS. R. 


811 


— 


Neb. II. 756 


f 


32 


n 


2 ] 


LfF.S.E. 


812 


— , 


21 (p) Draconis 


P 


55 20 


n 


3 18] 


1 vF. vS. IE. 


813 


— 


— — 


P 


36 1 


n 


1 14- 


1 z>F, vS. *'R. 


814 


26 


5 Ganum 


P 


15 


n 


32- 


1 z>F. S. er. 


815 


— 


7 Canum 


f 


18 48 


f 


22 • 


1 S. Stellar. 


816 




— — 


f 


25 11 


n 


* 33' 


1 eF. S. ZE. 


817 


— 


— — 


I 


26 43 


n 


45 


l cF. S. *F. 


818 


— 


— — 


f 


33 4 


I 


1 7 


1 cF. S. R. i^/6M. 



SH 



Dr. Herschel's Catalogue 



in. 



819 
820 



821 
822 
823 

824 
825 
826 

827 
828 

829 
830 
831 
832 

833 

834 
835 
836 

837 
838 

839 

840 

841 

842 

843 
844 

845 
846 

847 
848 

849 
850 



1790 
Mar. 8 



1789. 



Apr. 26' 



82 Ursa? 



10 



17 



18 



Stars. 



7(«)Hyd.Crat. 
39 Lyncis 



Hyd. L. C. 1039 

;7 Lyncis 

15 (f) Ursa? 

26 Ursa? 
74 Ursa? 
77 Ursa? 
17 Ursa? 



43 Ursa; 
66 Ursa? 

69 ($) Ursa? 

19 20 Ursse 
76' Ursa? 
69 Ursa? Hev. 

20 76 Ursa? 



P 
P 
P 

f 
P 
P 
I 
P 

P 
P 
P 

I 

P 

P 
P 
P 
P 
P 
P 
P 
P 
P 
I 
P 
P 
f 
P 



M. S. 



33 15 
29 17 



12 59 
6 23 

5 5 



7 26 
12 1 

5 55 

2 11 

2 1 

23 49 
10 40 
12 8 

9 39 

*34 3 

2 4 

82 37 

79 17 



75 

75 

72 

63 
16 

5 

19 
16" 

4 
7 
S7 
19 
23 
26 



32 
10 



/ 

22!/ 
56\f 

if 



8 

23 

1 



53 

53 

5 

53 
56 



D. M. 



12 

48 



7 

25 
1 

9 

3 1 
56 

29 

11 

30 

19 
23 

57 
43 
56 
52 



40 

15 

40 

28 

9 
39 

52 
2 

17 
23 

50 

13 
8 

17I1 



Description. 



vF. 

2fS stars at less than l'd. 
with f F. nebulosity be- 
tween therm. 

cF. Stellar. 

cF.pS. ill. IbM. 

cF.pL.R.vlbM. 

vF. vS. z'R. glbM. 
vF.S.R.bM.fofaSft. 
vF. S r. 

eF.vS.ffavSft. 
eF.pS.R.vgbM. Stellar. just 

p a t>S/£. 
eF. wS. R. bM. 
cF.pS.bM. 
vF. v$. 
vF. S. IE. 
vF. vS. 
eF. S. zF. 

eF. S. E. but nearly R. 
t^F. vS. maybe a patch of 

stars. 
eF. v S. 
eF. z>S. 
eF. wS. 
cF. cS. 
vY.S. 
vF. vS. R. 

f F. Stellar, np a S/h 
z^F. S. mE. 
t'F. S. E. par. 
cF. S. mE. very narrow. 
eF. v S. zF. 
t;F. f S. 
z>F. z>S. 
|vF./>S. 



of 500 new Nebula, and Clusters of Stars. 



&-i 



III. 


1790. 


Stars. 




M. S. 




VI. D. a 


Description. 


851 


Mar. 20 


y6 Ursas 


P 


25 25 


n 


3 43 * 


*F. S. iF. 


852 


— - 


— — __ 


P 


l6 38 


n 


3 12 1 


vF. Stellar, nfa S triangle of 
Bft. 


853 


Apr. 1 


go (<p) Ursas 


f 


8 55 


n 


1 35 ^ 


vF. S. vglbM. 


854 


Oct. 9 


72 Pegasi 


f 


15 8 


J 


D 232 


qvS close ft. with nebulosity 
between. 


%5 

S56 














f Two nebulas, both eF. Stel- 
| lar. dist. l'from 30°^* 
I to nf. 


}- 


— — 


f 


27 *5 


n 


O 3:: 1 


857 




7 Fornacis L. \ 
C. 285 - J 


P 


12 30 


I 


1 54 1 


vF.S.iF.lbM. 


858 


10 


6 Pegasi - 


P 


24, 40 


n 


43 1 


eF. pL. ill. vlbM. requires 
great attention to be seen. 


859 


—^ 


__ _ 


P 


7 S^n 


171 


l cF.vS.iR.mbM.nea.ra.vSft, 


860 


Nov. 2 


72 Pegasi 


P 


5 ] 9» 


1 71 


vF. S. IbM. 


861 


,-— 


— — 


f 


37 5o 


I 


171 


. eF. S. 


862 


8 


1 Lacertas Hev. 


P 


3 17 


n 


1 19 1 


£>F.jbL.z'R. r. 


863 


— 


— — 


f 


3 9 


n 


481 


. vF. vS. mbM. 


864 


— 


— . — 


f 


4 37 


n 


50 j 


. vF. S. raE. 75 »£/jf. 6M. 


865 


13 


26 Auriga? 


P 


1 9 


n 


1 311 


t z>F. vS. R- 6M. 


866 


26 


29 [mr) Androm. 


P 


27 37 


I 


20 ' 


l f F. r>S. The «£ corner of a 
square. 


867 


Dec. 6 


Mayer's Zod.i 
Cat. 20 - 1 


P 


49 5 9 


I 


1 39 


ieF.pS.iR.lbM. 


868 


— 


— — 


P 


39 35 


I 


42" 


ieF.pS.iF. 


86c, 


25 


4,4, Piscium 


f 


3 25 


n 


55 


t vF. vS. bM. p. and in the 
field with II. 854. nf. 2. 
Sjt. 


870 


, — , 


— — 


f 


12 48 


n 


49 


1 vF. S. zR. vgbM. 


871 


28 


Mayer's Zod. i 
Cat. 1,8 - J 


P 


8 1 


n 


1 44 


1 vF. S. R. vgbM. 


872 


, 


— . — 


P 


5 52 


n 


41 


1 i>F. riS. 6M. 


873 




~ ~ 


P 


5 3 2 


n 


39 


1 ^F, cL. In the field with the 
foregoing, and with II. 
860, 


874 


"'■""" 


57 Auriga? 


I 


17 5 6 


n 


1 50 


1 vF. vS. /E. 


875 


— 


— — 


I 


21 42 


I 


o"7 


1 vF. vS, 



SiS 



Dr. Herschel's Catalogue 



in. 



876 Dec. 2351 Piscium 



877 



1790. 



Stars. 



Feb. 23 2 6 Hy dree 



May 6 



24 



878 Apr. 

879 

880 

881 
882 
883 
884 
885 

886 
887 

888 
889 
890 
891 
892 

893 

1792 
894 Apr. 20 

895 
896 

1793 



2 14 (t) Ursas 
73 Ursas 



335 Ursae - 



9 Ursae min 
13(9/) Ursas min. 

37 (£) Bootis 



26 7 Serpentis 



2719 (|) Coronas 
28' 17 (<r) Coronas 
20 (V) Coronas 
25 Herculis 



30 



44 (vj) Herculis 
22 (f) Bootis 



J Feb. 4 34 (0) Gemin. 



897 
89« 

899 

900 

901 

902JMar.8 
903lApr. 6 

904I ~ 



}- 



/ 



M. 



18 Navis 
4 Draconis 



5 44 



73 56 

9 14 

2 39 
8 13 

21 51 

34 52 
4 2 4 1 
44 51 

3 44 

15 3 2 

6 41 

2 1 
8 9n 

3 4i 
2 5 
6 26 



D. M. 



n 



1 43 



o 22 



12 29 

!2 55 
16 45 



1 33 

15 18 
36 21 

10 36 n 
30 43 n 
23 25] » 



38 
12 
26* 

o 
g6 

22 

35 



o 20 



7 
52 
20 

37 

9 

8 



1 15 

o 47 
o 25 



3i 

17 



Description. 



vF.ph. iR.Jfa Sft whjch-is 
partly involved in the ne- 
bulosity. 

vF. iR. r. <z'd. almost of equal 

light throughout. 
vF. ch. R. mbM, near $'d. 
cF. S. iF. 
eF. S. 
z/F.S. 

t>F, />L. R. 6M. 
?F. t>S. ver. 300. 
fF. v S. with 300 cL, 
<?F. t>S. E. near par. 

{Two nebulas, both eF. vS. 
the p is the most n. dist. 
2 
<?F. z>S. R. with 300 ph. 

vF. S. R. vglbM. 

vF.pL.lE.lbM. 

eF. vS. R. IbM. 

eF.S.bM. 

eF. vS. iF. ver. 300. 

vF. vS. 
vF. vS. 
eF. S. vlbM. 



9 

32 
10 
24 



Two nebulae. The most n. 
andp.eF. S. The other 
eF. vS. dist. 4'. 
v F. S. nearly R. 6M. 
Two nebulas just prece- 
ding III. 703. Both eF. 
vF. IE. r. 6M. 
eF. S. iF. vlbU. 
eF. vS. E. mer. 



of goo new Nebulce, and Clusters of Stars, 



5*7 



in. 

9°5 
go6 

9°7 

908 

9°9 
9io 

911 

912 
9*3 
9H< 
9*5 
916 

917 
918 

919 
920 

921 
922 

923 

924 

925 
926 

927 

928 

9*9 
93° 
93 1 
932 



1793- 



Apr. 7 



8 



39 Ursas 
942 Ursa? 



May 5 



Sept. 6 



933 

934 

MDCCCII 



1794 

Apr. 1 



Stars. 



4 Draconis 
6 Draconis 



37 Ursas 



Hydr.L.C.i 179 
6 Hydras conti 
64 Virginis 



19 Bootis Hev. 
1393 (0 Virgin. 



53 Aquarii 



Georgian planet 



P 



M. S. 



37 3 
12 31 
16 26 

23 36 

39 i° 
15 47 

11 47 
o 59 
8 14 

10 29 

25 35 
48 48 

15 19 

15 10 

o 1 

19 23 

24 11 

35 14 



1 

11 

1 

*3 



25 

2 

18 

5 
o 20 

26 17 
9 25 

27 19 
12 23 

8 .50 



6" 



16 



11 



I 



D. M 



8 

8 

35 
10 

35 
19 

5 

27 

14 

2 

3 
39 

44 

47 
2 

1 

22 

11 

5 

27 

10 

17 

44 

5 

35 
18 

19 
11 



o 58 



Description. 



¥b. 



eF. vS. ver. 300. 

v F. E. 2'/, i'6. 

vF.F.npff. ii'Z, 

<?F. z>S. iR. »/&M. 

vF. vS. R. 

z>F. />L. zF. r. some of the 
stars visible. 

vF. cL. zF. 

?F. t>S. ver 300. 

z>F. z>S. 

vF. S. /E. 

r>F.S. 

<?F. vS. Stellar near a S/if. 

r Two nebulae. 

lBotht;F./>S. R./6M. 

vF. vS. near a z>S/£. 

eF. vS. E. near mer. 

eF.pL. E. 

i>F. z>S. 2z>S. stars in it. 

vF.vS.R.lbM. 

eF. S. r. ver. 300. 

cF. S. 

vF. S.fp.zcBft. 

vF. S. 

vF. S. 

vF. S. E. mer. 

^F. ver. 300. 

eF. S. z'R. 

eF. S. IE. fof a Sft.to which 
it seems almost to be at- 
tached, but is free from it. 
The star is the 1st of 3, 
making a S triangle. 

vF. S. R. 6M. 

vF. This nebula was seen 
at 9 h 45', sidereal time, the 



3X 



51 8 



Dr. Herschel's Catalogue 



III. 


1794. 


Stars. 




M. 


s. 




D. M. 5 


r Description. 


















telescope being out of the 
meridian. 


935 


Apr. 19 


12 (£) Hydrae 


















crateris 


/ 


15 


11 


w 


401 


. eF. S. bM. 


936 Oct. 15 


5 («) Cephei 


/ 


7 54 


» 


16] 


vF. er, 




1797 
















937 


Nov. 22 


Neb. I. 274 


/ 


25 


3 


« 


53 3 


vF. S. iR. bM. 


93 8 


Dec. 10 


A double st* 


P 


9 


5 


n 


lOl 


eF.pL,. z'F.* See I. 273. 


939 


— 


■ — — 


f 


4 





I 


35 ] 


ieF. S. 


94° 


12 


5 Dracon.Hev, 


P 


32 


24 


I 


49 ] 


1 vF. S. R. bM. 


94i 


— 


— — 


P 


8 


21 


n 


573 


1 vF. pS. 2 S nf stars make a 
a triangle with it. 


94 s 


— 


. — — 


f 


4 


16 


n 


59 1 


1 tfF. E. near mer. ver. 300. 


943 
944 


}- 


5 (a) Urssemi. 


f 


46 


2 


1 


281 


f Two nebulae. 

[Both z'F. z>S.r.dist. if par. 


945 


___ 


35 Draconis 


P 


47 


10 


I 


1 17] 


1 vF. S. E. n of a Sft. 


94 6 


20 


4 (6) Ursae mi. 


P 


29 


3i 


n 


1 57 ] 


l z/F. vS. R. 


947 


— 


— — 


P 


14 39 


n 


42- 


t vF. cL. iF. vlbM.fofapB. 


















fi- 


94 8 


— . 


— _ 


f 


2 


20 


n 


1 3 


l eF. vS. E. near mer. 


949 


___ 


, — — 


f 


14 44 


n 


2 29 


1 eF. S. IE. near par. 


95o 






I 


24 


18 


n 


1 13. 


t z'F. S. r. It is preceded by a 
S. patch ofjt which ap- 
pears almost like this ne- 
bula, but more resolved. 


95i 


— 


4 Cephei of 


















Bode's Cat. 


P 


21 


18 


I 


1 25 


1 eF. S. better with 320. 




1798 


















lDec.9 














fTvvo nebulae within 1' of 


95% 

953 


2 (7/) Ononis 


P 


10 


20 


I 


1 34 


1 \ each other; mer. Both 
I fF. vS. 


954 


10 


8 Ceti - 


J 


^7 


5 


f 
j 


1 15 


1 eF. S. 


955 


— 


21 Ceti 


P 


3 


46 


n 


4 


1 cF. vS. iR. 


95 ( > 


1799 


18 (e) Eridani 


P 


15 


21 


J 


53 


1 vF. vS. 2 or 3' n of 2SJL 


957 

958 


1 June 

J 2 9 


93 Herculis 


P 


4 
3 


3 

59 


n 


1 33 
1 37 


(Two nebulas. 
1 I Both z'F. vS. 



mios.Tra7u-MDCCC T I.Fla£eXV I.p. 518. 




J(Z&„3. 




3%ck£. 




*3fy'a„'7. 




P 



v" f' mm ' ' 1 -% / 

4 — - — ■ — ■ — .* ■■ — -<...„„ ,1/. / 

n - Vs ' ' //T 1 






^/Za-„8 




of 500 new Nebula?, and Clusters of Stars. 



519 



in. 



959 

960 
961 
962 

963 

9 6 5 
9 66 

967 
968 

9 6 9 

97o 

97i 
972 

973 

974 

975 

976 



1799. 



Dec. 19 



1801 
Apr. 2 



}- 



Nov. 28 
Dec. 6 

1802 
J Jan. 1 

May 21 



Stars. 



16 Eridani 

19 Eridani 



2o8(N)Caraelop. 
of Bode's Cat. 



50 (a) Ursa? 
16 (£) Ursas mi, 



22 (s) Ursas mi 



977 Sep. 26 
978 



2 (??) Coronas 

186 P. Camelop. 
of Bode's Cat, 



P 

P 

P 
P 

P 

P 
P 
P 
P 
I 



M. S. 



6 37 

1 19 

2 43 
20 51 



157 S 6 
119 54 

117 22 

118 o 

72 10 

37 3 1 

24 19 
20 34 

5 7 
14 15 



10 49 
26 50 



9 49 
33 19 



D. M 



O 26 



n 



n 



f 



13 

4 6> 
15 

16 
5 



56 
29 



l 52 



39 

28 

3 1 

10 

8 



o 37 



o 2 



1 S3 
o 5« 



Description. 



The 2d of 2 vF. vS. 1%'ffl. 

60. 

vF. vS. ver. 300. 
vF. vS. 
vF. vS.Jp. zpBft. 



eF. S, z'F. 

cF. S. Stellar, ver. 300. just 

p. a S/t. 
vF.vS. 
vF. vS. 
Two nebulas. The 1st vF. 

S. 
The 2d nf. the 1st *F. vS. 
eF. S. 
vF.ph. r. 
eF. vS. R. 
vF. v$. R. 6M. 
t;F. S. IE, mer. r. 
Two nebulas ; the preced- 
ing cF. S. 6M. the foil. 
-< vF. vS. it follows the 1st 
a few seconds, and is 3' 
more north. 
eF. S. iF. 



eF. vS. 300 confir. 
eF.pL. vlbM. just « of %/£. 



3 x * 



52 o 



Dr. Herschel's Catalogue 



Fourth Class. Planetary Nebula. 
Stars with Burs, with milky Chevelures, with short Rays, remarkable Shapes, &c. 



IV. 



59 Mar. 23 55 Ursas - 



60 



61 



6z 



63 



64 



65 



1789. 



Stars. 



Apr. 1 236 Ursas 



14 



64 (y) Ursae 



24|6g Ursa? Hev. 



1790 

Mar. 4 



6 Navis 



28 Monocerotis 



/ 



/ 



/ 



/ 



/ 



P 



M. 



4 5i 



8 $7 



3 56 



2 27 



1 24 



7 4 1 



5 1 49 



72 



/ 



/ 



» 



o 19 



1 25 



/ 



/ 



n 



D. M. 



o 23 



2 28 



1 33 



1 2 



o 26 



Description. 



dB.S.R.BN. The N is con- 
siderably well defined, and 
the chevelure vF. 

vB. R. Planetary, but very 
ill defined. The indis- 
tinctness on the edges is 
sufficiently extensive to 
make this a step between 
planetary neb. and those 
which are described 
vfmbM. 

cB. BrN with z>FE branches 
about 30 np ff. 7 or 8'/, 
4 or 5'b. 

cB. quite R. A large place in 
the middle is nearly of an 
equal brightness. To- 
wards the margin it is less 
bright. 

cB. cL. iR. er. vgmbM. 4' 
diam. I suppose, with a 
higher power, I might 
have seen the stars. 

A beautiful planetary nebu- 
la, of a considerable de- 
gree of brightness; not 
very well defined, about 
12 or 15" diam. 

A pretty considerable star, 
9 or 10m. visibly affect- 
ed with vF. nebulosity, 
of very little extent all 



of 500 new Nebula, and Clusters of Stars. 



521 



IV. 



1790. 



Stars, 



66' 



Mar. 18 



67 



68 



69 Nov. 30 



17 Ursae - 



66 Ursas - 



1945 Lyncis 



i 



26 Auriga 
Hevelii 



or 31 



P 



P 



u, 



16 29 



° 39 



4 15 



88 24 
24 59 



D. M. 



/ 



n 



3 6 



1 55 



44 



11 
26 



Description. 



around. A power of 300 
shewed the same, but gave 
a little more extent to the 
nebulosity. The2sd Mon- 
cerotis was quite free from 
nebulosity. 
A small star with apB. fan- 
shaped nebula. The star 
is on the p side of the di- 
verging chevelure, and 
seems to be connected 
with it. 
pB. ph. R. The greatest 
part of it equally B, then 
fading away p suddenly ; 
between 2 and 3' diam. 
vB. S. exactly R. BNM.and 
t;F. chev. vg. joining to 
the N. In a lower situa- 
tion the chev. might not 
be visible, and this neb. 
would then appear like an 
ill defined planetary one. 
A most singular phenome- 
non; Aft 8m. with a faint 
luminous atmosphere of a 
circular form, about 3' in 
diam. The star is perfect- 
ly in the centre, and the 
atmosphere is so diluted, 
faint, and equal through- 
out, that there can be no 
surmise of its consisting of 
stars, nor can there be a 
doubt of the evident con- 
nection between the at- 
mosphere and the star, 



Dr. Herschel's Catalogue 



IV. 



70 



71 



72 



73 



1790. 



Stars. 



1791 

Mar. 6 



May 24 



1792 
Sep. 15 



1793 
Sep. 6 



6 Draconis 



87 (I) Bootis 



34,Cygni - 



16 (O Cygni 



/ 



/ 



P 



f 



M. S. 



50 27 



16 5 



10 



2 51 



/ 



?z 



/ 



D. M 



o 27 



o 44 



o 



23 



Description. 



Another star, not much 
less in brightness, and in 
the same field with the 
above, was perfectly free 
from any such appear- 
ance. 

cB. R. almost equally B 
throughout, resembling a 
very ill defined planetary 
neb. about i'diam. 
star 7.6m. enveloped in 
extensive milky nebulo- 
sity. Another star 7m. is 
perfectly free from such 
appearance. 

A double star of the 8th 
magnitude, with a faint 
south - preceding milky 
ray joining to it, 8'/, and 
ii' broad. 

A bright point, a little ex- 
tended, like two points 
close to one another ; as 
bright as a star of the 8.9 
magnitude, surrounded by 
a very bright milky nebu- 
losity suddenly termina- 
ted, havingtheappearance 
of a planetary nebula with 
a lucid centre; the border 
however is not very well 
defined. It is perfectly 
round,and I suppose about 
half a minute in diam. It 



of 500 new Nebula, and Clusters of Stars. 



523 



IV. 



*793- 



1794 

74 Oct. 18 



75 



76 Sep 



1798 
it. 9 



77 



Dec. 19 



Stars. 



7 Cephei - 



7 Cephei 



3 (*?) Cephei 



16 Eridani 



/ 



/ 



M. S. 



24 57 



14 40 



10 31 



4 56 



n 



/ 



/ 



ft 



M. D. 



1 22 



46 



1 36 



o 14 



Description. 



is of a middle species, be- 
tween the planetary ne- 
bulae and nebulous stars, 
and is a beautiful pheno- 
menon. 

A star 7m. very much af- 
fected with nebulosity, 
which more than fills the 
field. It seems to extend 
to at least a degree all 
around ; smaller stars, 
such as 9 or 1 om . of which 
there are many, are per- 
fectly free from this ap- 
: pearance. 

A star 7.8m. is perfectly 
free from this appearance. 

Three stars about 9m. in- 
volved in nebulosity. The 
whole takes up a space of 
about i^'diam. other stars 
of the same size are free 
from nebulosity. 

cF. vL. iF. a sort of $NM. 
The nebulosity 6 or 7'. 
The N seems to consist 
of stars, the nebulosity is 
of the milky kind. It is a 
pretty object. 

A star about 9 or 10m. with 
a nebulous ray to the 
south-precedingside. The 
ray is about 1 J-' long. The 
star may not be connected 
with it. 



524 



Dr. Herschel's Catalogue 



IV. 



1801. 



Stars. 



78 Nov. 8 



8 Urseemin. of 
Bode's Cat. 



P 



M. S. 



25 o 



n 



D. M. 



O 12 



Description. 



[' 



cB. R. about if diarn. 
Somewhat approaching 
to a planetary nebula, 
with a strong hazy border. 



Fifth Class. Very large Nebula. 



v, 



45 



4 6 



1789. 



Apr. 12 



1790 
47 April i 



48 



49 



50 

51 



i74,8(/3)Ursa3 



Oct. g 



1798 

Mar. 4 



April 6 



Stars. 



64 (7) Ursas - 



30 (tp) Ursa? 

< Fornacis L. C. 

182 - - 



Dec. 2841 Persei Hev. 



e Pixidis Na. L. 
C. 831 - 

4 Draconis - 



/ 
/ 

/ 
/ 

/ 



M. S. 



O 9 

IO 4 

10 9 

8 7 

22 o 



35 s6 
14 48 



/ 



M. D. 



1 23 

41 

1 39 

O 2 

o i,5 



o 43 
o 20 



Description. 



cB. £F. E. mer. LBN. with 
F. branches 7 or 8'/, 5 or 
6'b. 

vB, wE. r. io'/, 2'6. There 
is an unconnected pretty 
bright star in the middle. 

vB. i»E. np ff. vgmbM. 8'/, 
a'6. 

»B. E. 75 # //. 8' long. A 
very bright nucleus, con- 
fined to a small part, or 
about 1' diam. 

6 or 7 small stars, with faint 
nebulosity between them, 
of considerable extent, 
and of an irregular figure. 



vF. vS. IE. xgfpnf. IbWL. 
8'1, 5 or 6'b. 

vF. mE. yd" npff. About 
25'/, and losing itself im- 
perceptibly, about 6 or 7' 
broad. 



of 500 new Nebula, and Clusters of Stars. 



fty f 



V. 


1801. 


Stars. 




M. S. 




D. M. 





Description. 


52 


Nov.28 


50 (a) Ursse 


p 


l 7 49 


ra 


1 30 


] 


cB. E. mer. r/g-fcM. About 
5'/. and 3' broad ; the ne- 
bulosity seems to be of* 
the milky kind; it loses 
itself imperceptibly all a- 
round. The whole breadth 
of the sweep seems to be 
affected with very faint 
nebulosity. 



Sixth Class. Very compressed and rich Clusters of Stars. 

Additional Tel. Cluster, com. compressed, 
Abbreviations.] sc. scattered, co. coarsely. 



VI. 



1790. 



$6 Mar. 4 



37 Feb 



38 
89 



179* 
23 



Aug.25 

*793 
Mar. 3 



Star s 



6 Navis 



26 Hydras - 



50 (y) Aquilaa 



£ Pixidis Naut. 
L. C. 777 - 



M. S. 



P 



P 



MDCCCII. 



8 45 



79 So 



14 50 



20 39 



/ 



n 



1 



I 



D. M. 



1 55 



1 18 



o 10. 



Description. 



A t>. com. cl. of S, and some 
1ft. E near mer. The 
most compressed part is 
about 87, and 2'6. with 
many scattered to a con- 
siderable distance. 

A v. com. and very rich cl. 
of stars. The stars are of 
2 sizes, some considerably 
L. and the rest next to 
invisible. The com. part 
5 or 6' in diam. 

6-B. S. z'F. er. Some of theft. 
are visible. 



A cl. of lft. considerably 
rich z'R. above 15' diam. 



3Y 



X26 



Dr. Herschel's Catalogue 



VI. 

40 



41 



42 



J 793- 



May 12 



1-797 
Dec. 1 2 



53 (1/) Serpentis 



1798 
Sep. 9 



Stars. 



35 Draconis - 



3 (,) Cephei 



P 



P 



M. S. 



48 17 



22 6 



13 26 



» 



y 



/ 



D. M, 



O 2 



1 7 



i 6 



Description. 



A very beautiful e com. cl. 
of JL extremely rich, 5 or 
6' in diam. gradually more 
compressed towards the 
centre. 

R. r. about 3' diam. tg-6M. 
I suppose it to be a clus- 
ter of stars extremely 
compressed. 300 confirms 
the supposition, and shews 
a few of the stars ; it must 
be immensely rich. 

A beautiful compressed cl. 
of Sft. extr. rich, of an 
i F. The preceding part of 
it is round, and branching 
out on the following side, 
both towards the n. and 
towards the /. 8 or 9' in 
diam. 



Seventh Class. Pretty much 


compressed Clusters of large or small Stars. 


VII. 


1788. 


Stars. 




M. S. 




D. M.lS 
1 


Description. 


56 


Dec. 16 


11 (jQ) Cassiop 


P 


9 57 


n 


2 6 


1 


A p. com. cl. of Sft. of se- 
veral sizes, cons. rich. E. 


57 
59 


3 1 

1790 

Mar. 4 

Sept. 11 


40 Auriga? - 

6 Navis 
18 ($) Cygni 


f 

f 
f 


8 28 

5 18 
1.8 38 


n 

f 
J 


1 25 
29 


1 

1 
1 


near par. 5 or 67. 
A compressed cl. of vS stars 
z'F. 6' diam. consid. rich. 

A p. com. and rich cl. of S 
stars zR. 7 or 8' diam. 

A v. rich cl. of Lft. conside- 
rably compressed, above 



of goo new Nebula, and Clusters of Stars. 



527 



VII. 



60 Dec. 28 



61 

62 

6$ 
64, 

65 



Aug. 21 



67 J 



1790. 



1793 

Mar, 



8 



66 Oct. 18 



1799 
lan. 30 



Stars. 



47 (x) Persei 
41 Persei Hev. 



19 Aquilae - 



3C 



Pixidis Naut, 
L. C. 777 - 



2 Navis 



7 Cephei - 



15 (V) Canis 



/ 



/ 



M. 



3 3° 
3 8 

o 26 

2 25 
20 55 

16 10 
16 45 

42 33 



D. M 



o 50 

56 

1 24 

24 

1 9 

38 

1 7 

o 14 



Description. 



15' diam. by the size of 
theft, it is situated in the 
milky-way, towards us. 

AL. cl. oicLft.p. com. and 
very rich. z'R. 7' diam. 

A beautiful cl. of hft. v rich, 
and considerably com. 
about 15' diam. 

A S. p. com. cl. of stars not 
very rich. 



A L. cl. of scattered Sft. zF. 
considerably rich. 

A L. cl. of ft. of a middling 
size, i E. considerably 
rich. The stars are chiefly 
in rows. 

A S. cl. of vS ft. considera- 
bly rich and compressed. 

A cl. of cons. com. vS and 
L. stars about 12' diam. 
considerably rich. 

A cl. of com. stars, consi- 
derably rich. 



sYs 



A3 8 



Dr. Herschel's Catalogue, &c. 



Eighth Class. Coarsely scattered Clusters of Stars. 



VIII 



79 



80 



82 
83 



84 
«5 



Dec. 16 



18 



*7 8 9 

July 18 

1790 
Sept. 11 

QO 



Dec. 28 



Stars. 



11 (|G) Cassiop 
1 Camelopar. 

5 Vulpeculee 

57 c yg ni - 

51 Cygni - 



33 («) Persei 
4,1 Persei Hev. 



1792 
86 Sept. 15 34 Cy 



87 
88 



1793 

Mar. 8 

1799 
Dec. 28 



gni 



2 Navis 



46 (|) Persei 



/ 



M. S. 



SO 3,5 



4* 3 6 

2 46 

1 o 

25 24 



9 14 
2 42 



9 43 

7 10 
27 *3 



D. M. 



W 



/ 



n 



1 5 
1 29 

a 4 

o 52 
o 1 



1 36 

O 2 



o 151 

15 

1 29 



Description. 



A coarsely sc. cl. of hft. 

mixed with smaller ones, 

not very rich. 
A cl. of S. stars, containing 

one large one, 10; 9m. 2; 

or 3' diam. not rich. 

A sc. cl. of chft. i¥. pretty 
rich, above 15' in extent. 

A L. cl. of fiS. stars of se- 
veral sizes. 

A cl. of sc. stars, above 15' 
diam. pretty rich, joining 
to the milky-way, or a 
projecting part of it. 

A cl. of Sft. not very rich. 

A coarsely sc. cl. of hft. 
pretty rich. 

A coarsely sc. cl. ofL stars,, 
of a right-angled triangu- 
lar shape. 

A small cl. of S. stars, not 
very rich. 

A cl. of coarsely sc. hft, 
about 15' diam. 



JPhilos Jmn s M T>CCCJ U J late WR.p.BiS . 




■ -y^jy^o . 




M. 



T xa,^2. 





w 



, /fBft.vire
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